256 results on '"MILKY-WAY"'
Search Results
2. The Gaia-ESO survey:Mapping the shape and evolution of the radial abundance gradients with open clusters
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L. Magrini, C. Viscasillas Vázquez, L. Spina, S. Randich, D. Romano, E. Franciosini, A. Recio-Blanco, T. Nordlander, V. D’Orazi, M. Baratella, R. Smiljanic, M. L. L. Dantas, L. Pasquini, E. Spitoni, G. Casali, M. Van der Swaelmen, T. Bensby, E. Stonkute, S. Feltzing, G. G. Sacco, A. Bragaglia, E. Pancino, U. Heiter, K. Biazzo, G. Gilmore, M. Bergemann, G. Tautvaišienė, C. Worley, A. Hourihane, A. Gonneau, and L. Morbidelli
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YOUNG OPEN CLUSTERS ,IRON ABUNDANCES ,POPULATION ASTROPHYSICS SPA ,FOS: Physical sciences ,Astronomy and Astrophysics ,CHEMICAL EVOLUTION ,Astrophysics - Astrophysics of Galaxies ,evolution [Galaxy] ,abundances [stars] ,OLD OPEN CLUSTERS ,Astronomi, astrofysik och kosmologi ,ELEMENT ABUNDANCES ,ATMOSPHERIC PARAMETERS ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,evolution [stars] ,Astronomy, Astrophysics and Cosmology ,MILKY-WAY ,general [open clusters and associations] ,PLANETARY-NEBULAE ,GALACTIC METALLICITY GRADIENT - Abstract
The spatial distribution of elemental abundances and their time evolution are among the major constraints to disentangle the scenarios of formation and evolution of the Galaxy. We used the sample of open clusters available in the final release of the Gaia-ESO survey to trace the Galactic radial abundance and abundance to iron ratio gradients, and their time evolution. We selected member stars in 62 open clusters, with ages from 0.1 to about 7~Gyr, located in the Galactic thin disc at Galactocentric radii from about 6 to 21~kpc. We analysed the shape of the resulting [Fe/H] gradient, the average gradients [El/H] and [El/Fe] combining elements belonging to four different nucleosynthesis channels, and their individual abundance and abundance ratio gradients. We also investigated the time evolution of the gradients dividing open clusters in three age bins. The[Fe/H] gradient has a slope of -0.054 dex~kpc-1. We saw different behaviours for elements belonging to different channels. We found that the youngest clusters in the inner disc have lower metallicity than their older counterpart and they outline a flatter gradient. We considered some possible explanations, including the effects of gas inflow and migration. We suggested that it might be a bias introduced by the standard spectroscopic analysis producing lower metallicities in low gravity stars. To delineate the shape of the `true' gradient, we should limit our analysis to stars with low surface gravity logg>2.5 and xi, 25 pages, 14 figures and 4 tables in the main text, 3 figures and 7 tables in the Appendix. Accepted for publication in A&A
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- 2023
3. Dusty Starbursts Masquerading as Ultra-high Redshift Galaxies in JWST CEERS Observations
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Jorge A. Zavala, Véronique Buat, Caitlin M. Casey, Steven L. Finkelstein, Denis Burgarella, Micaela B. Bagley, Laure Ciesla, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Maximilien Franco, E. F. Jiménez-Andrade, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Aurélien Le Bail, E. J. Murphy, Casey Papovich, Sandro Tacchella, Stephen M. Wilkins, Itziar Aretxaga, Peter Behroozi, Jaclyn B. Champagne, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Lisa J. Kewley, Dale D. Kocevski, Allison Kirkpatrick, Jennifer M. Lotz, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Guang Yang, L. Y. Aaron Yung, Omar Almaini, Ricardo O. Amorín, Marianna Annunziatella, Pablo Arrabal Haro, Bren E. Backhaus, Guillermo Barro, Eric F. Bell, Rachana Bhatawdekar, Laura Bisigello, Fernando Buitrago, Antonello Calabrò, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Nikko J. Cleri, Seth H. Cohen, Justin W. Cole, Kevin C. Cooke, M. C. Cooper, Asantha R. Cooray, Luca Costantin, Isabella G. Cox, Darren Croton, Romeel Davé, Alexander de la Vega, Avishai Dekel, David Elbaz, Vicente Estrada-Carpenter, Vital Fernández, Keely D. Finkelstein, Jonathan Freundlich, Seiji Fujimoto, Ángela García-Argumánez, Jonathan P. Gardner, Eric Gawiser, Carlos Gómez-Guijarro, Yuchen Guo, Timothy S. Hamilton, Nimish P. Hathi, Benne W. Holwerda, Michaela Hirschmann, Marc Huertas-Company, Taylor A. Hutchison, Kartheik G. Iyer, Anne E. Jaskot, Saurabh W. Jha, Shardha Jogee, Stéphanie Juneau, Intae Jung, Susan A. Kassin, Peter Kurczynski, Rebecca L. Larson, Gene C. K. Leung, Arianna S. Long, Ray A. Lucas, Benjamin Magnelli, Kameswara Bharadwaj Mantha, Jasleen Matharu, Elizabeth J. McGrath, Daniel H. McIntosh, Aubrey Medrano, Emiliano Merlin, Bahram Mobasher, Alexa M. Morales, Jeffrey A. Newman, David C. Nicholls, Viraj Pandya, Marc Rafelski, Kaila Ronayne, Caitlin Rose, Russell E. Ryan, Paola Santini, Lise-Marie Seillé, Ekta A. Shah, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Elizabeth R. Stanway, Amber N. Straughn, Harry I. Teplitz, Brittany N. Vanderhoof, Jesús Vega-Ferrero, Weichen Wang, Benjamin J. Weiner, Christopher N. A. Willmer, Stijn Wuyts, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
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Astrofísica ,1ST BILLION YEARS ,Near infrared astronomy ,FOS: Physical sciences ,DEEP-FIELD-NORTH ,Starburst galaxies ,Millimeter astronomy ,ALMA SPECTROSCOPIC SURVEY ,STAR-FORMING GALAXIES ,Galaxy photometry ,Dust continuum emission ,SUBMILLIMETER GALAXIES ,Astronomy and Astrophysics ,MASSIVE GALAXIES ,Emission line galaxies ,Galaxies ,MULTIWAVELENGTH PROPERTIES ,Astrophysics - Astrophysics of Galaxies ,Lyman-break galaxies ,Luminous infrared galaxies ,Astronomía ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,High-redshift galaxies ,MILKY-WAY ,James Webb Space Telescope ,INTERSTELLAR DUST ,Submillimeter astronomy ,COSMOLOGY LEGACY SURVEY - Abstract
Lyman Break Galaxy (LBG) candidates at z>10 are rapidly being identified in JWST/NIRCam observations. Due to the (redshifted) break produced by neutral hydrogen absorption of rest-frame UV photons, these sources are expected to drop out in the bluer filters while being well detected in redder filters. However, here we show that dust-enshrouded star-forming galaxies at lower redshifts (z10 LBGs, representing potential contaminants in LBG candidate samples. First, we analyze CEERS-DSFG-1, a NIRCam dropout undetected in the F115W and F150W filters but detected at longer wavelengths. Combining the JWST data with (sub)millimeter constraints, including deep NOEMA interferometric observations, we show that this source is a dusty star-forming galaxy (DSFG) at z~5.1. We also present a tentative 2.6sigma SCUBA-2 detection at 850um around a recently identified z~16 LBG candidate in the same field and show that, if the emission is real and associated with this candidate, the available photometry is consistent with a z~5 dusty galaxy with strong nebular emission lines despite its blue near-IR colors. Further observations on this candidate are imperative to mitigate the low confidence of this tentative submillimeter emission and its positional uncertainty. Our analysis shows that robust (sub)millimeter detections of NIRCam dropout galaxies likely imply z=4-6 redshift solutions, where the observed near-IR break would be the result of a strong rest-frame optical Balmer break combined with high dust attenuation and strong nebular line emission, rather than the rest-frame UV Lyman break. This provides evidence that DSFGs may contaminate searches for ultra high-redshift LBG candidates from JWST observations., Published in The Astrophysical Journal Letters (updated to match the published version)
- Published
- 2023
4. The Gaia-ESO survey: placing constraints on the origin of r-process elements
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M. Van der Swaelmen, C. Viscasillas Vázquez, G. Cescutti, L. Magrini, S. Cristallo, D. Vescovi, S. Randich, G. Tautvaišienė, V. Bagdonas, T. Bensby, M. Bergemann, A. Bragaglia, A. Drazdauskas, F. Jiménez-Esteban, G. Guiglion, A. Korn, T. Masseron, R. Minkeviiūtė, R. Smiljanic, L. Spina, E. Stonkutė, S. Zaggia, Van der Swaelmen, M., Viscasillas Vázquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaišienė, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jiménez-Esteban, F., Guiglion, G., Korn, A., Masseron, T., Minkevičiūtė, R., Smiljanic, R., Spina, L., Stonkutė, E., and Zaggia, S.
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CLUSTERS TRUMPLER 20 ,FOS: Physical sciences ,NEUTRON-STAR MERGERS ,Astrophysics ,Astrophysics of Galaxies ,Astrophysics Solar and Stellar Astrophysics ,HEAVY-ELEMENTS ,STELLAR POPULATIONS ,Astrophysic ,PROCESS NUCLEOSYNTHESIS ,Astronomi, astrofysik och kosmologi ,Astronomy, Astrophysics and Cosmology ,STOCHASTIC CHEMICAL EVOLUTION ,Astrophysics of Galaxie ,GIANT BRANCH STARS ,Solar and Stellar Astrophysics (astro-ph.SR) ,abundances [Galaxy] ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,abundances [stars] ,ALPHA-RICH STARS ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,MILKY-WAY ,CAPTURE ELEMENTS ,general [open clusters and associations] ,disk [Galaxy] - Abstract
A renewed interest about the origin of \emph{r}-process elements has been stimulated by the multi-messenger observation of the gravitational event GW170817, with the detection of both gravitational waves and electromagnetic waves corresponding to the merger of two neutron stars. Such phenomenon has been proposed as one of the main sources of the \emph{r}-process. However, the origin of the \emph{r}-process elements at different metallicities is still under debate. We aim at investigating the origin of the \emph{r}-process elements in the Galactic thin disc population. From the sixth internal data release of the \emph{Gaia}-ESO we have collected a large sample of Milky Way thin- and thick-disc stars for which abundances of Eu, O, and Mg are available. The sample consists of members of 62 open clusters, located at a Galactocentric radius from $\sim 5$ kpc to $\sim 20$ kpc in the disc, in the metallicity range $[-0.5, 0.4]$ and covering an age interval from 0.1 to 7 Gy, and about 1300 Milky Way disc field stars in the metallicity range $[-1.5, 0.5]$. We compare the observations with the results of a chemical evolution model, in which we varied the nucleosynthesis sources for the three considered elements. Our main result is that Eu in the thin disc is predominantly produced by sources with short lifetimes, such as magneto-rotationally driven SNe. There is no strong evidence for additional sources at delayed times. Our findings do not imply that there cannot be a contribution from mergers of neutron stars in other environments, as in the halo or in dwarf spheroidal galaxies, but such a contribution is not needed to explain Eu abundances at thin disc metallicities., 20 pages, accepted for publication in A&A
- Published
- 2023
5. The Pristine survey -- XX: GTC follow-up observations of extremely metal-poor stars identified from Pristine and LAMOST
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Anke Arentsen, David S Aguado, Federico Sestito, Jonay I González Hernández, Nicolas F Martin, Else Starkenburg, Pascale Jablonka, and Zhen Yuan
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search ,espadons ,abundances ,carbon ,ancient ,FOS: Physical sciences ,Astronomy and Astrophysics ,stars: population ii ,low-metallicity stars ,galaxy survey pigs ,Astrophysics - Astrophysics of Galaxies ,stars: chemically peculiar ,galaxy: halo ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,evolution ,stellar streams ,techniques: spectroscopic ,milky-way ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Ultra metal-poor stars ([Fe/H] < -4.0) are very rare, and finding them is a challenging task. Both narrow-band photometry and low-resolution spectroscopy have been useful tools for identifying candidates, and in this work we combine both approaches. We cross-matched metallicity-sensitive photometry from the Pristine survey with the low-resolution spectroscopic LAMOST database, and re-analysed all LAMOST spectra with [Fe/H]_Pristine < -2.5. We find that ~1/3rd of this sample (selected without [Fe/H]_Pristine quality cuts) also have spectroscopic [Fe/H] < -2.5. From this sample, containing many low signal-to-noise (S/N) spectra, we selected eleven stars potentially having [Fe/H] < -4.0 or [Fe/H] < -3.0 with very high carbon abundances, and we performed higher S/N medium-resolution spectroscopic follow-up with OSIRIS on the 10.4m Gran Telescopio Canarias (GTC). We confirm their extremely low metallicities, with a mean of [Fe/H] = -3.4 and the most metal-poor star having [Fe/H]= -3.8. Three of these are clearly carbon-enhanced metal-poor (CEMP) stars with +1.65 < [C/Fe] < +2.45. The two most carbon-rich stars are either among the most metal-poor CEMP-s stars or the most carbon-rich CEMP-no stars known, the third is likely a CEMP-no star. We derived orbital properties for the OSIRIS sample and find that only one of our targets can be confidently associated with known substructures/accretion events, and that three out of four inner halo stars have prograde orbits. Large spectroscopic surveys may contain many hidden extremely and ultra metal-poor stars, and adding additional information from e.g. photometry as in this work can uncover them more efficiently and confidently., 13 pages, accepted for publication in MNRAS
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- 2023
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6. Dust depletion of metals from local to distant galaxies I. Peculiar nucleosynthesis effects and grain growth in the ISM
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Christina Konstantopoulou, Annalisa De Cia, Jens-Kristian Krogager, Cédric Ledoux, Pasquier Noterdaeme, Johan P. U. Fynbo, Kasper E. Heintz, Darach Watson, Anja C. Andersen, Tanita Ramburuth-Hurt, Iris Jermann, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
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INTERSTELLAR ABUNDANCES ,absorption lines [quasars] ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,GAMMA-RAY BURST ,STAR-FORMATION ,abundances [galaxies] ,Magellanic Clouds ,Astrophysics::Solar and Stellar Astrophysics ,DAMPED LY-ALPHA ,Astrophysics::Galaxy Astrophysics ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,ISM [galaxies] ,extinction ,ELEMENTAL ABUNDANCES ,ZINC ABUNDANCES ,GALACTIC CHEMICAL EVOLUTION ,abundances [Galaxy] ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,quasars: absorption lines ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,Galaxy: abundances ,MILKY-WAY ,galaxies: abundances ,LARGE-MAGELLANIC-CLOUD ,Astrophysics::Earth and Planetary Astrophysics ,dust ,dust, extinction ,HIGH-REDSHIFT ,galaxies: ISM - Abstract
Large fractions of metals are missing from the observable gas-phase in the interstellar medium (ISM) because they are incorporated into dust grains, a phenomenon called dust depletion. The study of dust depletion in the ISM is important to investigate the origin and evolution of metals and cosmic dust. Here we aim at characterizing the dust depletion of several metals from the Milky Way to distant galaxies. We collect ISM metal column densities from absorption-line spectroscopy in the literature, and in addition, we determine Ti and Ni column densities from a sample of 70 damped Lyman-$\alpha$ absorbers (DLAs) towards quasars, observed with UVES/VLT. We use ISM relative abundances to estimate the dust depletion of 18 metals (C, P, O, Cl, Kr, S, Ge, Mg, Si, Cu, Co, Mn, Cr, Ni, Al, Ti, Zn and Fe) for different environments (the Milky Way, the Magellanic Clouds (MCs), DLAs towards quasars and towards gamma-ray bursts). We observe linear relations between the depletion of each metal and the strength of dust depletion, which we trace with the observed [Zn/Fe]. In the neutral ISM of the MCs we find small deviations from linearity observed as an overabundance of the $\alpha$-elements Ti, Mg, S and an underabundance of Mn. The deviations disappear if we assume that all OB stars observed towards the MCs in our sample have an $\alpha$-element enhancement and Mn underabundance. This may imply that the MCs have been recently enriched in $\alpha$-elements, potentially due to recent bursts of star formation. The observed strong correlations of the depletion sequences of the metals all the way from low metallicity QSO-DLAs to the Milky Way suggest that cosmic dust has a common origin, independently of the star formation history, which varies significantly between these different galaxies. This supports the importance of grain growth in the ISM as a significant process of dust production., Comment: 30 pages, 35 figures, 12 tables, Accepted for publication in A&A, Abstract abridged for arXiv
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- 2022
7. Mapping the aliphatic hydrocarbon content of interstellar dust in the Galactic plane
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B Günay, M G Burton, M Afşar, and T W Schmidt
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dust extinction ,infrared: ISM ,Organic-Molecules ,astrochemistry ,Evolution ,FOS: Physical sciences ,Extinction Law ,Astronomy and Astrophysics ,Iras 18511+0146 ,Milky-Way ,Astrophysics - Astrophysics of Galaxies ,ISM: abundances ,Carbon ,techniques: photometric ,Abundance ,Gas ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,methods: observational ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Embedded Sources ,L-Band - Abstract
We implement a new observational method for mapping the aliphatic hydrocarbon content in the solid phase in our Galaxy, based on spectrophotometric imaging of the 3.4 mu m absorption feature from interstellar dust. We previously demonstrated this method in a field including the Galactic Centre cluster. We applied the method to a new field in the Galactic Centre where the 3.4 mu m absorption feature has not been previously measured and we extended the measurements to a field in the Galactic plane to sample the diffuse local interstellar medium, where the 3.4 mu m absorption feature has been previously measured. We have analysed 3.4 mu m optical depth and aliphatic hydrocarbon column density maps for these fields. Optical depths are found to be reasonably uniform in each field, without large source-to-source variations. There is, however, a weak trend towards increasing optical depth in a direction towards b = 0 degrees in the Galactic Centre. The mean value of column densities and abundances for aliphatic hydrocarbon were found to be about several x 10(18) cm(-2) and several tens x 10(-6), respectively for the new sightlines in the Galactic plane. We conclude that at least 10-20 per cent of the carbon in the Galactic plane lies in aliphatic form., Scientific and Technological Research Council of Turkey (TUBITAK); Australian Research Council [CE170100026, DP190103151]; University of New South Wales (UNSW); National Aeronautics and Space Administration, BG would like to thank to The Scientific and Technological Research Council of Turkey (TUBITAK) for their support in this work through the 2214/A International Research Fellowship Programme. TWS is supported by the Australian Research Council (CE170100026 and DP190103151). The University of New South Wales (UNSW) seeded this work through the award of a Faculty interdisciplinary grant.; This research has made use of the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology.
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- 2022
8. Optical and near-infrared observations of the Fried Egg Nebula; Multiple shell ejections on a 100 yr timescale from a massive yellow hypergiant
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V. Graham, N. L. J. Cox, Eric Lagadec, C. Wichittanakom, R. D. Oudmaijer, F. Millour, G. Banyard, S. H. J. Wallstrom, John H. Black, Albert A. Zijlstra, E. Koumpia, Ryszard Szczerba, Sebastien Muller, K. M. Ababakr, H. Van Winckel, W. J. de Wit, Michel Hillen, and Jacco Vink
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010504 meteorology & atmospheric sciences ,Hypergiant ,H-ALPHA ,FOS: Physical sciences ,Astrophysics ,Astronomy & Astrophysics ,Computer Science::Digital Libraries ,01 natural sciences ,LUMINOUS BLUE VARIABLES ,Photometry (optics) ,Atmospheric radiative transfer codes ,0103 physical sciences ,DATA REDUCTION ,RESOLVED SPECTROSCOPY ,Yellow hypergiant ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Physics ,Nebula ,Science & Technology ,RHO-CASSIOPEIAE ,Near-infrared spectroscopy ,Astrophysics::Instrumentation and Methods for Astrophysics ,mass-loss [stars] ,Astronomy and Astrophysics ,Observable ,RED SUPERGIANT IRC+10420 ,AGB and post-AGB [stars] ,imaging [stars] ,Physics::History of Physics ,interferometric [techniques] ,Wavelength ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,evolution [stars] ,Physical Sciences ,MILKY-WAY ,O-STARS ,MAGELLANIC-CLOUD ,HIGH-RESOLUTION SPECTROSCOPY ,individual: IRAS 17163-3907 [stars] - Abstract
Context. The fate of a massive star during the latest stages of its evolution is highly dependent on its mass-loss rate/geometry and therefore knowing the geometry of the circumstellar material close to the star and its surroundings is crucial. Aims. We aim to study the nature (i.e. geometry, rates) of mass-loss episodes. In this context, yellow hypergiants are great targets. Methods. We analyse a large set of optical/near-infrared data, in spectroscopic and photometric (X-shooter/VLT), spectropolarimetric (ISIS/WHT), and interferometric GRAVITY-AMBER/VLTI) modes, toward the yellow hypergiant IRAS 17163-3907. We present the first model-independent reconstructed images of IRAS 17163-3907 at these wavelengths at milli-arcsecond scales. Lastly, we apply a 2D radiative transfer model to fit the dereddened photometry and the radial profiles of published VISIR images at 8.59 {\mu}m, 11.85 {\mu}m and 12.81 {\mu}m simultaneously, adopting the revised Gaia distance (DR2). Results. The interferometric observables around 2 {\mu}m show that the Br{\gamma} emission is more extended and asymmetric than the Na i and the continuum emission. In addition to the two known shells surrounding IRAS 17163-3907 we report on the existence of a third hot inner shell with a maximum dynamical age of only 30 yr. Conclusions. The interpretation of the presence of Na i emission at closer distances to the star compared to Br{\gamma} has been a challenge in various studies. We argue that the presence of a pseudophotosphere is not needed, but it is rather an optical depth effect. The three observed distinct mass-loss episodes are characterised by different mass-loss rates and can inform the theories on mass-loss mechanisms, which is a topic still under debate. We discuss these in the context of photospheric pulsations and wind bi-stability mechanisms., Comment: 26 pages, 22 Figures, 6 tables, accepted for publication in A&A. Original abstract will be available after publication
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- 2022
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9. The Metallicity Distribution Function in Outer Halo Fields of Simulated Elliptical Galaxies Compared to Observations of NGC 5128
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Ena Choi, Jeremiah P. Ostriker, Michaela Hirschmann, Rachel S. Somerville, and Thorsten Naab
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stars ,smoothed particle hydrodynamics ,FOS: Physical sciences ,driven disk winds ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,telescope photometry ,y-2 isochrones ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,giant branch ,evolution ,Astrophysics::Solar and Stellar Astrophysics ,ngc-5128 ,Astrophysics::Earth and Planetary Astrophysics ,milky-way ,Astrophysics::Galaxy Astrophysics ,stellar population gradients - Abstract
Stellar metallicity distribution functions (MDF) have been measured for resolved stellar populations in the outer halos of many galaxies in nearby groups. Among them, the MDF of NGC 5128, the central giant elliptical in the Centaurus group, provides essential constraints for theories of massive galaxy formation and hierarchical assembly. To investigate the formation and chemical evolution history of the outer halo of giant elliptical galaxies, we examine the chemical properties of three zoom-in high resolution cosmological hydrodynamical simulations of an NGC 5128-like giant elliptical galaxy and compare their outer halo MDFs to the observed one of NGC 5128. Even though the simulated galaxies have different merging histories and age distributions, all predicted MDFs are in good qualitative agreement with the observed one. The median metallicity of the simulated galaxies is on average $\rm [M/H]=-0.41 \pm 0.06$ compared to the observed value of $\rm [M/H]=-0.38 \pm 0.02$ for NGC 5128, and the dispersion in metallicity is $\sim 0.77$ dex for both observed and simulated galaxies. We investigate the origin of the stars ending up in the outer halo field of simulated galaxies and show that most have an `accreted' origin, formed in other small galaxies and later accreted in mergers. Only $\sim 15$ percent of the stars are formed `in situ' within the main progenitor of galaxy and radially migrate outwards. We show that the contribution of metal-rich in situ stars is sub-dominant in the outer halos of our simulated galaxies, but can be prominent in the inner regions., 16 pages, 9 figures, Accepted for publication in ApJ
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- 2022
10. How much metal did the first stars provide to the ultra-faint dwarfs?
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Mahsa Sanati, Fabien Jeanquartier, Yves Revaz, and Pascale Jablonka
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smoothed particle hydrodynamics ,chemical enrichment ,galaxy: abundances ,formation history ,cosmological simulations ,FOS: Physical sciences ,stars: population iii ,mass-metallicity relation ,Astronomy and Astrophysics ,galaxies: dwarf ,Astrophysics::Cosmology and Extragalactic Astrophysics ,galaxy formation ,Astrophysics - Astrophysics of Galaxies ,methods: numerical ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::Solar and Stellar Astrophysics ,high-resolution spectroscopy ,spheroidal galaxy ,poor stars ,milky-way ,Astrophysics::Galaxy Astrophysics - Abstract
Numerical simulations of dwarf galaxies have so far failed to reproduce the observed metallicity-luminosity relation, down to the regime of ultra-faint dwarfs (UFDs). We address this issue by exploring how the first generations of metal-free stars (Pop III) could help increase the mean metallicity ([Fe/H]) of those small and faint galaxies. We ran zoom-in chemo-dynamical simulations of 19 halos extracted from a Λ Cold Dark Matter (CDM) cosmological box and followed their evolution down to redshift z = 0. Models were validated not only on the basis of galaxy global properties, but also on the detailed investigation of the stellar abundance ratios ([α/Fe]). We identified the necessary conditions for the formation of the first stars in mini-halos and derived constraints on the metal ejection schemes. The impact of Pop III stars on the final metallicity of UFDs was evaluated by considering different stellar mass ranges for their initial mass function (IMF), the influence of pair-instability supernovae (PISNe), and their energetic feedback, as well as the metallicity threshold that marks the transition from the first massive stars to the formation of low-mass long-lived stars. The inclusion of Pop III stars with masses below 140 M⊙, and a standard IMF slope of −1.3 does increase the global metallicity of UFDs, although these are insufficient to resolve the tension with observations. The PISNe with progenitor masses above 140 M⊙ do allow the metal content of UFDs to further increase. However, as PISNe are very rare and sometimes absent in the faintest UFDs, they have a limited impact on the global faint end of the metallicity-luminosity relation. Despite a limited number of spectroscopically confirmed members in UFDs, which make the stellar metallicity distribution of some UFDs uncertain, our analysis reveals that this is essentially the metal-rich tail that is missing in the models. The remaining challenges are thus both observational and numerical: (i) to extend high-resolution spectroscopy data samples and confirm the mean metallicity of the faintest UFDs; and (ii) to explain the presence of chemically enriched stars in galaxies with very short star formation histories.
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- 2023
11. The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and Hα Emission for 49 PHANGS Galaxies
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Hsi-An Pan, Eva Schinnerer, Annie Hughes, Adam Leroy, Brent Groves, Ashley Thomas Barnes, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Yixian Cao, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Cinthya N. Herrera, I-Ting Ho, Ralf S. Klessen, J. M. Diederik Kruijssen, Philipp Lang, Daizhong Liu, Rebecca McElroy, Sharon E. Meidt, Eric J. Murphy, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Erik Rosolowsky, Toshiki Saito, Francesco Santoro, Andreas Schruba, Jiayi Sun, Neven Tomičić, Antonio Usero, Dyas Utomo, Thomas G. Williams, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
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[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,FORMATION EFFICIENCY ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,ATOMIC GAS ,DIFFUSE IONIZED-GAS ,Physics and Astronomy ,CO-TO-H-2 CONVERSION FACTOR ,Space and Planetary Science ,LUMINOSITY FUNCTION ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,MILKY-WAY ,Astrophysics::Earth and Planetary Astrophysics ,MAGELLANIC-CLOUD ,GIANT MOLECULAR CLOUDS ,UNCERTAINTY PRINCIPLE ,Astrophysics::Galaxy Astrophysics ,SDSS-IV MANGA - Abstract
The relative distribution of molecular gas and star formation in galaxies gives insight into the physical processes and timescales of the cycle between gas and stars. In this work, we track the relative spatial configuration of CO and H$\alpha$ emission at high resolution in each of our galaxy targets, and use these measurements to quantify the distributions of regions in different evolutionary stages of star formation: from molecular gas without star formation traced by H$\alpha$ to star-forming gas, and to HII regions. The large sample, drawn from the Physics at High Angular resolution in Nearby GalaxieS ALMA and narrowband H$\alpha$ (PHANGS-ALMA and PHANGS-H$\alpha$) surveys, spans a wide range of stellar mass and morphological types, allowing us to investigate the dependencies of the gas-star formation cycle on global galaxy properties. At a resolution of 150 pc, the incidence of regions in different stages shows a dependence on stellar mass and Hubble type of galaxies over the radial range probed. Massive and/or earlier-type galaxies exhibit a significant reservoir of molecular gas without star formation traced by H$\alpha$, while lower-mass galaxies harbor substantial HII regions that may have dispersed their birth clouds or formed from low-mass, more isolated clouds. Galactic structures add a further layer of complexity to relative distribution of CO and H$\alpha$ emission. Trends between galaxy properties and distributions of gas traced by CO and H$\alpha$ are visible only when the observed spatial scale is $\ll$ 500 pc, reflecting the critical resolution requirement to distinguish stages of star formation process., Comment: 60 pages, 22 figures, 9 tables, accepted for publication in The Astrophysical Journal
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- 2022
12. DarkFlux: A new tool to analyze indirect-detection spectra of next-generation dark matter models
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Antonio Boveia, Linda M. Carpenter, Boyu Gao, Taylor Murphy, and Emma Tolley
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density ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astronomy and Astrophysics ,maddm ,numerical tools ,dark matter ,High Energy Physics - Phenomenology ,High Energy Physics - Phenomenology (hep-ph) ,Space and Planetary Science ,indirect detection ,indirect searches ,milky-way ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present DARKFLUX, a software tool designed to analyze indirect-detection signatures for next-generation models of dark matter (DM) with multiple annihilation channels. Version 1.0 of this tool accepts user-generated models with 2 -> 2 tree-level dark matter annihilation to pairs of Standard Model (SM) particles and analyzes DM annihilation to gamma rays. The tool consists of three modules, which can be run in a loop in order to scan over DM mass if desired, (I) The annihilation fraction module calls an internal installation of MADDM, a dark matter phenomenology plugin for the Monte Carlo event generator MADGRAPH5_AMC@NLO, to compute the thermally averaged cross section (i) for each annihilation channel chi chi((chi) over bar, chi(dagger)) -> i is an element of {SM, SM}. The module then computes the fractional annihilation rate (annihilation fraction) into each channel., (II) The flux module combines the flux spectrum from each annihilation channel, weighted by the appropriate annihilation fractions, to compute the total flux at Earth due to DM annihilation. In DARKFLUX v1.0, this module specifically computes the gamma-ray flux for each channel using the publicly available PPPC4DMID tables., (III) The analysis module compares the total flux to observational data and computes the upper limit at 95% confidence level (CL) on the total thermally averaged DM annihilation cross section. In DARKFLUX v1.0, this module compares the total gamma-ray flux to a joint-likelihood analysis of fifteen dwarf spheroidal galaxies (dSphs) analyzed by the Fermi-LAT collaboration., DARKFLUX v1.0 automatically provides data tables and can plot the output of these three modules. In this manual, we briefly motivate this indirect-detection computer tool and review the essential DM physics. We then describe the several modules of DARKFLUX in greater detail. Finally, we show how to install and run DARKFLUX and provide two worked examples demonstrating its capabilities. DARKFLUX is available on GitHub at https://github.com/carpenterphysics/DarkFlux. (C) 2022 Elsevier B.V. All rights reserved.
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- 2022
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13. The ALPINE-ALMA [CII] survey: dust attenuation curves at z=4.4-5.5
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Médéric Boquien, Véronique Buat, Denis Burgarella, Sandro Bardelli, Matthieu Béthermin, Andreas Faisst, Michele Ginolfi, Nimish Hathi, Gareth Jones, Anton Koekemoer, Brian Lemaux, Desika Narayanan, Michael Romano, Daniel Schaerer, Daniela Vergani, Giovanni Zamorani, Elena Zucca, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), and Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.)
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LEGACY SURVEY ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,H-ALPHA ,IRX-BETA RELATION ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,FAR-ULTRAVIOLET ,TO 3 ,LYMAN-BREAK GALAXIES ,galaxies: high-redshift ,[SDU]Sciences of the Universe [physics] ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,STAR-FORMING GALAXIES ,MILKY-WAY ,Astrophysics::Solar and Stellar Astrophysics ,HIGH-REDSHIFT ,MAIN-SEQUENCE ,high-redshift [galaxies] ,Astrophysics::Galaxy Astrophysics - Abstract
There is now ample evidence that dust is already present in abundance at high z. However, given the faintness of distant galaxies in the optical and the NIR, datasets are still limited and how the dust affects the emerging radiation of galaxies at very high redshift is not yet fully understood. Using the ALPINE survey, our objective is to quantify the dust attenuation properties in galaxies at z=4.4-5.5, and in particular the shape of their attenuation curve. Using the CIGALE code, we model the stellar populations and their interaction with the dust in order to measure some of the physical properties of a subsample of 23 main-sequence ALPINE galaxies. We find that the attenuation curves span a broad range of properties, from curves that are much steeper than the SMC extinction curve, to shallower than the starburst attenuation curve. The shape of the attenuation curves strongly depends on the V-band attenuation. Galaxies with the lowest attenuation also present the steepest curves. The steepness of such curves is probably the consequence of the combination of the intrinsic physical properties of the dust, the relative distribution of stars and dust in the interstellar medium, and the differential reddening. The broad range of attenuation curves found at z~5 shows that no single attenuation curve is appropriate for main sequence galaxies and that assuming a fixed curve can lead to large errors, for instance in the interpretation and use of the IRX-beta diagram, if SED modeling is not feasible. Great caution should be exercised when correcting high redshift galaxies for the presence of dust using the UV slope beta as it can affect the estimation of both SFR and stellar mass even at low V-band attenuation due to the steepness of the attenuation curve. However, when SED modeling can be used, the impact of the choice of the attenuation curve on the SFR and the stellar mass is limited., Comment: 20 pages, 14 figures. Accepted for publication in A&A
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- 2022
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14. The ALMA REBELS survey
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A Ferrara, L Sommovigo, P Dayal, A Pallottini, R J Bouwens, V Gonzalez, H Inami, R Smit, R A A Bowler, R Endsley, P Oesch, S Schouws, D Stark, M Stefanon, M Aravena, E da Cunha, I De Looze, Y Fudamoto, L Graziani, J Hodge, D Riechers, R Schneider, H S B Algera, L Barrufet, A P S Hygate, I Labbé, C Li, T Nanayakkara, M Topping, P van der Werf, Astronomy, Ferrara, A, Sommovigo, L, Dayal, P, Pallottini, A, J Bouwens, R, Gonzalez, V, Inami, H, Smit, R, A Bowler, R A, Endsley, R, Oesch, P, Schouws, S, Stark, D, Stefanon, M, Aravena, M, da Cunha, E, De Looze, I, Fudamoto, Y, Graziani, L, Hodge, J, Riechers, D, Schneider, R, B Algera, H S, Barrufet, L, S Hygate, A P, Labb('(e)), I, Li, C, Nanayakkara, T, Topping, M, and van der Werf, P
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Methods - analytical ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics - astrophysics of galaxies ,Astrophysics - cosmology and nongalactic astrophysics ,data analysis ,REDSHIFT ,Data analysis ,FOS: Physical sciences ,MASS ,Infrared - ISM ,methods: analytical ,analytical [methods] ,ATTENUATION ,Settore FIS/05 - Astronomia e Astrofisica ,galaxies: high-redshift ,STAR-FORMING GALAXIES ,TEMPERATURE ,QC ,Galaxies - high-redshift ,QB ,infrared: ISM ,UV LUMINOSITY FUNCTIONS ,ISM [infrared] ,Astronomy and Astrophysics ,ISM: dust ,extinction ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Extinction ,BRIGHT END ,EVOLUTION ,ISM - dust ,EXTINCTION ,Physics and Astronomy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,dust, extinction [ISM] ,MILKY-WAY ,high-redshift [galaxies] ,data analysi - Abstract
We analyse FIR dust continuum measurements for 14 galaxies ($z\approx 7$) in the ALMA REBELS LP to derive their physical properties. Our model uses three input data: (a) the UV spectral slope, $\beta$, (b) the observed UV continuum flux at $1500$A, $F_{\rm UV}$, (c) the observed continuum flux at $\approx 158\mu$m, $F_{158}$, and considers Milky Way (MW) and SMC extinction curves, along with different dust geometries. We find that REBELS galaxies have (28-90.5)% of their star formation obscured; the total (UV+IR) star formation rates are in the range $31.5 < {\rm SFR}/ (M_\odot {\rm yr}^{-1}) < 129.5$. The sample-averaged dust mass and temperature are $(1.3\pm 1.1)\times 10^7 M_\odot$ and $52 \pm 11$ K, respectively. In some galaxies dust is abundant (REBELS-14, $M'_d \approx 3.4 \times 10^7 M_\odot$), or hot (REBELS-18, $T'_d \approx 67$ K). The dust distribution is compact ($ 1 M_\odot$. With the SFR predicted by the model and a MW extinction curve, REBELS galaxies detected in [CII] nicely follow the local $L_{\rm CII}-$SFR relation, and are approximately located on the Kennicutt-Schmidt relation. The sample-averaged gas depletion time is of $0.11\, y_P^{-2}$ Gyr, where $y_P$ is the ratio of the gas-to-stellar distribution radius. For some systems a solution simultaneously matching the observed ($\beta, F_{\rm UV}, F_{158}$) values cannot be found. This occurs when the index $I_m = (F_{158}/F_{\rm UV})/(\beta-\beta_{\rm int})$, where $\beta_{\rm int}$ is the intrinsic UV slope, exceeds $I_m^*\approx 1120$ for a MW curve. For these objects we argue that the FIR and UV emitting regions are not co-spatial, questioning the use of the IRX-$\beta$ relation., Comment: 22 pages, 7 figures, accepted by MNRAS. Comments welcome
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- 2022
15. An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt law
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Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, and Martino Romaniello
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classical cepheids ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,period-luminosity relation ,variable-stars ,delta cephei ,large-magellanic-cloud ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,host galaxy ngc-4258 ,theoretical-models ,hubble-space-telescope ,key project ,milky-way - Abstract
The Cepheid period-luminosity (PL) relation (or Leavitt law) has served as the first rung of the most widely used extragalactic distance ladder and is central to the determination of the local value of the Hubble constant ($H_0$). We investigate the influence of metallicity on Cepheid brightness, a term that significantly improves the overall fit of the distance ladder, to better define its wavelength dependence. To this aim, we compare the PL relations obtained for three Cepheid samples having distinct chemical composition (in the Milky Way and Magellanic Clouds) and focusing on the use of improved and recent data while covering a metallicity range of about 1 dex. We estimate the metallicity effect (hereafter $\gamma$) in 15 filters from mid-IR to optical wavelengths, including five Wesenheit indices, and we derive a significant metallicity term in all filters, in agreement with recent empirical studies and models, in the sense of metal-rich Cepheids being brighter than metal-poor ones. We describe the contribution of various systematic effects in the determination of the $\gamma$ term. We find no evidence of $\gamma$ changing over the wavelength range $0.5-4.5 \, \rm \mu m$, indicating that the main influence of metallicity on Cepheids is in their luminosity rather than color. Finally, we identify factors that sharpen the empirical constraints on the metallicity term over past studies, including corrections for the depth of the Magellanic Clouds, better-calibrated Cepheid photometry, improved Milky Way extinction estimates, and revised and expanded metallicity measurements in the LMC., Comment: Accepted to ApJ
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- 2022
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16. A 0.9% Calibration of the Galactic Cepheid luminosity scale based on Gaia DR3 data of open clusters and Cepheids
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Reyes, Mauricio Cruz and Anderson, Richard I. I.
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classical cepheids ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astronomy and Astrophysics ,parallax zero-point ,data release 3 ,radial-velocities ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Solar and Stellar Astrophysics ,large-magellanic-cloud ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,parallaxes ,astrometry ,chemical-composition ,hubble-space-telescope ,period-luminosity ,milky-way ,Solar and Stellar Astrophysics (astro-ph.SR) ,fundamental parameters ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We have conducted a search for open clusters in the vicinity of classical Galactic Cepheids based on high-quality astrometry from the third data release (DR3) of the ESA mission Gaia to improve the calibration of the Leavitt law (LL). Our approach requires no prior knowledge of existing clusters, allowing us to both detect new host clusters and cross-check previously reported associations. Our Gold sample consists of 34 Cepheids residing in 28 open clusters, including 27 fundamental mode and 7 overtone Cepheids. Three new bona fide cluster Cepheids are reported (V0378 Cen, ST Tau, and GH Lup) and the host cluster identifications for three others (VW Cru, IQ Nor, and SX Vel) are corrected. The fraction of Cepheids occurring in open clusters within 2 kpc of the Sun is $f_{CC,2kpc} = 0.088^{+0.029}_{-0.019}$. By combining cluster and field Cepheids, we calibrate the LL for several individual photometric passbands, together with reddening-free Wesenheit magnitudes based on Gaia and HST photometry, while solving for the residual offset applicable to Cepheid parallaxes, $\Delta \varpi_{\mathrm{Cep}}$. The most direct comparison of our results with the SH0ES distance ladder yields excellent ($0.3\sigma$) agreement for both the absolute magnitude of a 10d solar metallicity Cepheid in the near-IR HST Wesenheit magnitudes, $M_{H,1}^W=-5.914\pm 0.017$ mag, and the residual parallax offset, $\Delta \varpi_{\mathrm{Cep}}=-13 \pm 5\,\mu$as. Using the larger sample of 26 Gold cluster Cepheids and $225$ MW Cepheids with recent Gaia DR3 astrometry and photometry, we determine at solar metallicity $M_{G,1}^W = -6.004 \pm 0.019$\,mag and $\Delta \varpi_{\mathrm{Cep}}=-19 \pm 3\,\mu$as. These results mark the currently most accurate absolute calibrations of the Cepheid luminosity scale based purely on observations of MW Cepheids., Comment: 24 pages, Version accepted in A&A
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- 2022
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17. [Mg/Fe] ratios in the solar neighbourhood: stellar yields and chemical evolution scenarios
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Marco Palla, Pablo Santos-Peral, Alejandra Recio-Blanco, and Francesca Matteucci
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IA SUPERNOVAE ,DATA RELEASE ,abundances [Galaxy] ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,GALACTIC ARCHAEOLOGY ,Astrophysics - Astrophysics of Galaxies ,GIANT BRANCH PHASE ,evolution [Galaxy] ,DELAYED GAS INFALL ,ALPHA-RICH STARS ,Physics and Astronomy ,nuclear reactions, nucleosynthesis, abundances ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,GAIA-ESO SURVEY ,MILKY-WAY ,AMBRE PROJECT ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,disk [Galaxy] ,MASSIVE STARS ,Astrophysics::Galaxy Astrophysics - Abstract
Context. The [Mg/Fe] abundance ratios are a fundamental fossil signature to trace the chemical evolution of the disc. Despite of the huge observational and theoretical effort, discrepancies between models and data are still present and several explanations have been put forward to explain the [$\alpha$/Fe] bimodality. Aims. In this work, we take advantage of a new AMBRE:HARPS dataset, which provides new and more precise [Mg/Fe] estimations, as well as reliable stellar ages for a subsample of stars, to study the evolution of the solar neighbourhood. Methods. The above data are compared with detailed chemical evolution models for the Milky Way, exploring the most used prescriptions for stellar yields and different formation scenarios for the Galactic disc, i.e. the delayed two-infall and the parallel model, also including prescriptions for stellar radial migration. Results. We see that most of the stellar yields struggle to reproduce the observed trend of the data and that semi-empirical yields are still the best to describe the [Mg/Fe] evolution in the thick and thin discs. In particular, most of the yields still predict a steeper decrease of the [Mg/Fe] ratio at high metallicity than what is shown by the data. The bulk of the data are well reproduced by the parallel and two-infall scenarios, but both scenarios have problems in explaining the most metal-rich and metal-poor tails of the low-$\alpha$ data. These tails can be explained in light of radial migration from inner and outer disc regions, respectively. Conclusions. Despite of the evidence of stellar migration, it is difficult to estimate the actual contribution of stars from other parts of the disc to the solar vicinity. However, the comparison between data and models suggests that peculiar histories of star formation, such as that of the two-infall model, are still needed to reproduce the observed distribution of stars., Comment: 16 pages, 16 figures. Accepted for publication in Astronomy and Astrophysics (A&A)
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- 2022
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18. The Gaia-ESO Survey: Old super-metal-rich visitors from the inner Galaxy
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M. L. L. Dantas, R. Smiljanic, R. Boesso, H. J. Rocha-Pinto, L. Magrini, G. Guiglion, G. Tautvaišienė, G. Gilmore, S. Randich, T. Bensby, A. Bragaglia, M. Bergemann, G. Carraro, P. Jofré, and S. Zaggia
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SOLAR NEIGHBORHOOD ,STELLAR ABUNDANCE ,F-DWARF ,abundances [Galaxy] ,FOS: Physical sciences ,Astronomy and Astrophysics ,CHEMICAL EVOLUTION ,kinematics and dynamics [Galaxy] ,Astrophysics - Astrophysics of Galaxies ,evolution [Galaxy] ,abundances [stars] ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,stellar content [Galaxy] ,MILKY-WAY ,KINEMATICS ,THICK ,RADIAL MIGRATION ,STARS ,Solar and Stellar Astrophysics (astro-ph.SR) ,GALACTIC DISK - Abstract
We report the identification of a set of old super metal-rich dwarf stars with orbits of low eccentricity that reach a maximum height from the Galactic plane between ~0.5-1.5 kpc. We discuss their properties to understand their origins. We use data from the internal data release 6 of the Gaia-ESO Survey. We selected stars observed at high resolution with abundances of 21 species of 18 individual elements. We apply hierarchical clustering to group the stars with similar chemical abundances within the complete chemical abundance space. According to their chemical properties, this set of super metal-rich stars can be arranged into five subgroups. Four seem to follow a chemical enrichment flow, where nearly all abundances increase in lockstep with Fe. The fifth subgroup shows different chemical characteristics. All subgroups have the following features: median ages of the order of 7-9 Gyr, Solar or sub-Solar [Mg/Fe] ratios, maximum height between 0.5-1.5 kpc, low eccentricities, and a detachment from the expected metallicity gradient with guiding radius. The high metallicity of our stars is incompatible with a formation in the Solar neighbourhood. Their dynamic properties agree with theoretical expectations that these stars travelled from the inner Galaxy due to blurring and, most importantly, to churning. We suggest that most of this population's stars originated in the Milky Way's inner regions (inner disc and/or the bulge) and later migrated to the Solar neighbourhood. The region from where the stars originated had a complex chemical enrichment history, with contributions from supernovae types Ia and II and possibly asymptotic giant branch stars., Comment: 18 pages, 13 figures. Accepted for publication in A&A. Version after language proofs. The catalogue remains to be released. Abridged abstract to fit arxiv's requirements
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- 2022
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19. The Gaia -ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy
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S. Randich, G. Gilmore, L. Magrini, G. G. Sacco, R. J. Jackson, R. D. Jeffries, C. C. Worley, A. Hourihane, A. Gonneau, C. Viscasillas Vazquez, E. Franciosini, J. R. Lewis, E. J. Alfaro, C. Allende Prieto, T. Bensby, R. Blomme, A. Bragaglia, E. Flaccomio, P. François, M. J. Irwin, S. E. Koposov, A. J. Korn, A. C. Lanzafame, E. Pancino, A. Recio-Blanco, R. Smiljanic, S. Van Eck, T. Zwitter, M. Asplund, P. Bonifacio, S. Feltzing, J. Binney, J. Drew, A. M. N. Ferguson, G. Micela, I. Negueruela, T. Prusti, H.-W. Rix, A. Vallenari, A. Bayo, M. Bergemann, K. Biazzo, G. Carraro, A. R. Casey, F. Damiani, A. Frasca, U. Heiter, V. Hill, P. Jofré, P. de Laverny, K. Lind, G. Marconi, C. Martayan, T. Masseron, L. Monaco, L. Morbidelli, L. Prisinzano, L. Sbordone, S. G. Sousa, S. Zaggia, V. Adibekyan, R. Bonito, E. Caffau, S. Daflon, D. K. Feuillet, M. Gebran, J. I. Gonzalez Hernandez, G. Guiglion, A. Herrero, A. Lobel, J. Maiz Apellaniz, T. Merle, Š. Mikolaitis, D. Montes, T. Morel, C. Soubiran, L. Spina, H. M. Tabernero, G. Tautvaišiene, G. Traven, M. Valentini, M. Van der Swaelmen, S. Villanova, N. J. Wright, U. Abbas, V. Aguirre Børsen-Koch, J. Alves, L. Balaguer-Nunez, P. S. Barklem, D. Barrado, S. R. Berlanas, A. S. Binks, A. Bressan, R. Capuzzo-Dolcetta, L. Casagrande, L. Casamiquela, R. S. Collins, V. D'Orazi, M. L. L. Dantas, V. P. Debattista, E. Delgado-Mena, P. Di Marcantonio, A. Drazdauskas, N. W. Evans, B. Famaey, M. Franchini, Y. Frémat, E. D. Friel, X. Fu, D. Geisler, O. Gerhard, E. A. Gonzalez Solares, E. K. Grebel, M. L. Gutierrez Albarran, D. Hatzidimitriou, E. V. Held, F. Jiménez-Esteban, H. Jönsson, C. Jordi, T. Khachaturyants, G. Kordopatis, J. Kos, N. Lagarde, L. Mahy, M. Mapelli, E. Marfil, S. L. Martell, S. Messina, A. Miglio, I. Minchev, A. Moitinho, J. Montalban, M. J. P. F. G. Monteiro, C. Morossi, N. Mowlavi, A. Mucciarelli, D. N. A. Murphy, N. Nardetto, S. Ortolani, F. Paletou, J. Palouš, E. Paunzen, J. C. Pickering, A. Quirrenbach, P. Re Fiorentin, J. I. Read, D. Romano, N. Ryde, N. Sanna, W. Santos, G. M. Seabroke, A. Spagna, M. Steinmetz, E. Stonkuté, E. Sutorius, F. Thévenin, M. Tosi, M. Tsantaki, J. S. Vink, N. Wright, R. F. G. Wyse, M. Zoccali, J. Zorec, D. B. Zucker, N. A. Walton, Universidad de Alicante. Departamento de Física Aplicada, Astrofísica Estelar (AE), Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
astro-ph.SR ,astro-ph.GA ,FOS: Physical sciences ,Techniques: spectroscopic ,Surveys ,fundamental parameters [Stars] ,VELOCITY DISPERSION PROFILES ,spectroscopic [Techniques] ,Astronomi, astrofysik och kosmologi ,Astronomy, Astrophysics and Cosmology ,LITHIUM DEPLETION ,TRUMPLER 20 ,Solar and Stellar Astrophysics (astro-ph.SR) ,Stars: fundamental parameters ,general [Open clusters and associations] ,Stars: abundances ,Astronomy and Astrophysics ,Open clusters and associations: general ,INNER-DISK ,CHEMICAL ABUNDANCES ,Astrophysics - Astrophysics of Galaxies ,GAMMA VELORUM CLUSTER ,Astrophysics - Solar and Stellar Astrophysics ,[SDU]Sciences of the Universe [physics] ,Space and Planetary Science ,SURVEY MEMBERSHIP PROBABILITIES ,Astrophysics of Galaxies (astro-ph.GA) ,SURVEY GALACTIC EVOLUTION ,abundances [Stars] ,6TH DATA RELEASE ,MILKY-WAY ,Catalogs - Abstract
Full list of authors: Randich, S.; Gilmore, G.; Magrini, L.; Sacco, G. G.; Jackson, R. J.; Jeffries, R. D.; Worley, C. C.; Hourihane, A.; Gonneau, A.; Vazquez, C. Viscasillas; Franciosini, E.; Lewis, J. R.; Alfaro, E. J.; Allende Prieto, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; Francois, P.; Irwin, M. J.; Koposov, S. E.; Korn, A. J.; Lanzafame, A. C.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Van Eck, S.; Zwitter, T.; Asplund, M.; Bonifacio, P.; Feltzing, S.; Binney, J.; Drew, J.; Ferguson, A. M. N.; Micela, G.; Negueruela, I; Prusti, T.; Rix, H-W; Vallenari, A.; Bayo, A.; Bergemann, M.; Biazzo, K.; Carraro, G.; Casey, A. R.; Damiani, F.; Frasca, A.; Heiter, U.; Hill, V; Jofre, P.; de Laverny, P.; Lind, K.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Sbordone, L.; Sousa, S. G.; Zaggia, S.; Adibekyan, V; Bonito, R.; Caffau, E.; Daflon, S.; Feuillet, D. K.; Gebran, M.; Gonzalez Hernandez, J., I; Guiglion, G.; Herrero, A.; Lobel, A.; Maiz Apellaniz, J.; Montes, D.; Morel, T.; Soubiran, C.; Spina, L.; Tabernero, H. M.; Traven, G.; Valentini, M.; Van der Swaelmen, M.; Villanova, S.; Wright, N. J.; Abbas, U.; Borsen-Koch, V. Aguirre; Alves, J.; Balaguer-Nunez, L.; Barklem, P. S.; Barrado, D.; Berlanas, S. R.; Binks, A. S.; Bressan, A.; Capuzzo-Dolcetta, R.; Casagrande, L.; Casamiquela, L.; Collins, R. S.; D'Orazi, V; Dantas, M. L. L.; Debattista, V. P.; Delgado-Mena, E.; Di Marcantonio, P.; Drazdauskas, A.; Evans, N. W.; Famaey, B.; Franchini, M.; Fremat, Y.; Friel, E. D.; Fu, X.; Geisler, D.; Gerhard, O.; Solares, E. A. Gonzalez; Grebel, E. K.; Gutierrez Albarran, M. L.; Hatzidimitriou, D.; Held, E., V; Jimenez-Esteban, F.; Jonsson, H.; Jordi, C.; Khachaturyants, T.; Kordopatis, G.; Kos, J.; Lagarde, N.; Mahy, L.; Mapelli, M.; Marfil, E.; Martell, S. L.; Messina, S.; Miglio, A.; Minchev, I; Moitinho, A.; Montalban, J.; Monteiro, M. J. P. F. G.; Morossi, C.; Mowlavi, N.; Mucciarelli, A.; Murphy, D. N. A.; Nardetto, N.; Ortolani, S.; Paletou, F.; Palous, J.; Paunzen, E.; Pickering, J. C.; Quirrenbach, A.; Fiorentin, P. Re; Read, J., I; Romano, D.; Ryde, N.; Sanna, N.; Santos, W.; Seabroke, G. M.; Spagna, A.; Steinmetz, M.; Stonkute, E.; Sutorius, E.; Thevenin, F.; Tosi, M.; Tsantaki, M.; Vink, J. S.; Wright, N.; Wyse, R. F. G.; Zoccali, M.; Zorec, J.; Zucker, D. B.; Walton, N. A., Context. In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey, the only one performed on a 8m class telescope, was designed to target 100 000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. Aims. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. Methods. We made use of the information recorded and archived in the observing blocks; during the observing runs; in a number of relevant documents; in the spectra and master catalogue of spectra; in the parameters delivered by the analysis nodes and the working groups; in the final catalogue; and in the science papers. Based on these sources, we critically analyse and discuss the output and products of the Survey, including science highlights. We also determined the average metallicities of the open clusters observed as science targets and of a sample of clusters whose spectra were retrieved from the ESO archive. Results. The Gaia-ESO Survey has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110 000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by the Gaia-ESO consortium and the community, with many highlight results achieved. Conclusions. The final catalogue will be released through the ESO archive in the first half of 2022, including the complete set of advanced data products. In addition to these results, the Gaia-ESO Survey will leave a very important legacy, for several aspects and for many years to come. © ESO 2022., Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes ID 188.B-3002, 193-B-0936, and 197.B-1074. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF-Osservatorio Astrofisico di Arcetri. Public access to the data products is via the ESO Archive, and the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF PRIN and Ministero dell’ Universitá e della Ricerca (MUR) in the form of the grant “Premiale VLT 2012” and “Premiale Mitic”. This work was partly supported by the INAF grant for mainstream projects: “Enhancing the legacy of the Gaia-ESO Survey for open cluster science”. The project presented here benefited in development from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. R. Smiljanic acknowledges support from the National Science Centre, Poland (2014/15/B/ST9/03981). F.J.E. acknowledges financial support from the Spanish MINECO/FEDER through the grant AYA2017-84089 and MDM-2017-0737 at Centro de Astrobiología (CSIC-INTA), Unidad de Excelencia Mar a de Maeztu, and from the European Union’s Horizon 2020 research and innovation programme under Grant Agreement no. 824064 through the ESCAPE - The European Science Cluster of Astronomy & Particle Physics ESFRI Research Infrastructures project. T.B. was funded by the “The New Milky Way” project grant from the Knut and Alice Wallenberg Foundation. S.R.B. acknowledges support by the Spanish Government under grants AYA2015-68012-C2-2-P and PGC2018-093741-B-C21/C22 (MICIU/AEI/FEDER, UE). W.J.S. acknowledges CAPES for a PhD studentship. J.M.A. acknowledges support from the Spanish Government Ministerio de Ciencia e Innovaciόn through grants AYA2013-40611-P, AYA2016-75931-C2-2-P, and PGC2018-095049-B-C22. T.M. and others from STAR institute, Liege, Belgium are grateful to Belgian F.R.S.-FNRS for support, and are also indebted for an ESA/PRODEX Belspo contract related to the Gaia Data Processing and Analysis Consortium and for support through an ARC grant for Concerted Research Actions financed by the Federation Wallonie-Brussels. This research has been partially supported by the ASI-INAF contract 2014-049-R.O: “Realizzazione attività tecniche/scientifiche presso ASDC” (PI Angelo Antonelli). V.A.acknowledges the support from Fundação para a Ciência e Tecnologia (FCT) through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. AJK acknowledges support by the Swedish National Space Agency (SNSA). AB acknowledges support by ANID, – Millennium Science Initiative Program – NCN19_171, and FONDECYT regular 1190748. E.M. acknowledges financial support from the Spanish State Research Agency (AEI) through project MDM-2017-0737 Unidad de Excelencia “María de Maeztu” – Centro de Astrobiología (CSIC-INTA). T.Z. acknowledges financial support of the Slovenian Research Agency (research core funding no. P1-0188) and the European Space Agency (Prodex Experiment Arrangement No. C4000127986). P.J. acknowledges support FONDECYT Regular 1200703. The work of I.N. is partially supported by the Spanish Government Ministerio de Ciencia, Innovaciόn y Universidades under grant PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). Funding for this work has been provided by the ARC Future Fellowship FT160100402. CAP acknowledges financial support from the Spanish Government through research grants MINECO AYA 2014-56359-P, MINECO AYA2017-86389-P, and MICINN PID2020-117493GB-I00. S.F. was supported by the grants 2011-5042 and 2016- 03412 from the Swedish Research Council and the project grant “The New Milky Way” from the Knut and Alice Wallenberg Foundation. CASU is supported through STFC grants: ST/H004157/1, ST/J00541X/1, ST/M007626/1, ST/N005805/1, ST/T003081/1. Work reported here benefited from support through the GREAT-ITN FP7 project Grant agreement ID: 264895. DKF acknowledges funds from the Alexander von Humboldt Foundation in the framework of the Sofja Kovalevskaja Award endowed by the Federal Ministry of Education and Research and the grant 2016-03412 from the Swedish Research Council. A.H. acknowledges support from the Spanish Government Ministerio de Ciencia e Innovaciόn and ERD Funds through grants PGC-2018-091 3741-B-C22 and CEX2019-000920-S. X.F. acknowledge the support of China Postdoctoral Science Foundation 2020M670023. M.L.L. Dantas acknowledges the Polish NCN grant number 2019/34/E/ST9/00133. Part of this work was funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A09). M.Z. acknowledge support from the National Agency for Research and Development (ANID) grants: FONDECYT Regular 1191505, Millennium Institute of Astrophysics ICN12-009, BASAL Center for Astrophysics and Associated Technologies AFB-170002. R.B. acknowledges support from the project PRIN-INAF 2019 “Spectroscopically Tracing the Disk Dispersal Evolution”. HMT acknowledges financial support from the Agencia Estatal de Investigaciόn of the Ministerio de Ciencia, Innovaciόn y Universidades through projects PID2019-109522GB-C51,54/AEI/10.13039/501100011033, and the Centre of Excellence “María de Maeztu” award to Centro de Astrobiología (MDM-2017-0737). JIGH acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) project AYA2017-86389-P, and also from the Spanish MICINN under 2013 Ramøn y Cajal program RYC-2013-14875. V.P.D. is supported by STFC Consolidated grant ST/R000786/1. N.L. acknowledges financial support from “Programme National de Physique Stellaire” (PNPS) and the “Programme National Cosmology et Galaxies (PNCG)” of CNRS/INSU, France. A.R.C. is supported in part by the Australian Research Council through a Discovery Early Career Researcher Award (DE190100656). Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. PSB is Supported by the Swedish Research Council through individual project grants with contract Nos. 2016-03765 and 2020-03404. A.M. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 772293 - project ASTEROCHRONOMETRY). J.P. was supported by the project RVO: 67985815. E.D.M. acknowledges the support from FCT through the research grants UIDB/04434/2020 & UIDP/04434/2020 and through Investigator FCT contract IF/00849/2015/CP1273/CT0003. This work was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018-095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia “María de Maeztu”) through grant CEX2019-000918-M. S.L.M. acknowledges the support of the UNSW Scientia Fellowship program and the Australian Research Council through Discovery Project grant DP180101791. G.T. acknowledges financial support of the Slovenian Research Agency (research core funding no. P1-0188) and the European Space Agency (Prodex Experiment Arrangement No. C4000127986). S.G.S. acknowledges the support from FCT through Investigador FCT contract no. CEECIND/00826/2018 and POPH/FSE (EC). H.G.L. acknowledges financial support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) - Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A04). This work was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018-095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia “María de Maeztu”) through grant CEX2019-000918-M. T.K. is supported by STFC Consolidated grant ST/R000786/1. M.V. acknowledges the support of the Deutsche Forschungsgemeinschaft (DFG, project number: 428473034). T.M. is supported by a grant from the Fondation ULB. We acknowledge financial support from the Universidad Complutense de Madrid (UCM) and by the Spanish Ministerio de Ciencia, Innovaciόn y Universidades, Ministerio de Economía y Competitividad, from project AYA2016-79425-C3-1-P and PID2019-109522GB-C5[4]/AEI/10.13039/501100011033. U.H. acknowledges support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). D.G. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofίsica y Tecnologías Afines (CATA) BASAL grant AFB-170002. D.G. also acknowledges financial support from the Direcciόn de Investigaciόn y Desarrollo de la Universidad de La Serena through the Programa de Incentivo a la Investigaciόn de Académicos (PIA-DIDULS). A. Lobel acknowledges support in part by the Belgian Federal Science Policy Office under contract no. BR/143/A2/BRASS. We acknowledge financial support from the Universidad Complutense de Madrid (UCM) and by the Spanish Ministerio de Ciencia, Innovaciόn y Universidades, Ministerio de Economía y Competitividad, from project AYA2016-79425-C3-1-P and PID2019-109522GB-C5[4]/AEI/10.13039/501100011033. AM acknowledges the support from the Portuguese Fundação para a Ciência e a Tecnologia (FCT) through the Portuguese Strategic Programme UID/FIS/00099/2019 for CENTRA. T.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) through the Spanish State Research Agency, under the Severo Ochoa Program 2020-2023 (CEX2019-000920-S). E.J.A. acknowledges funding from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709).
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- 2022
20. Quantifying the information impact of future searches for exoplanetary biosignatures
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Claudio Grimaldi and Amedeo Balbi
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life ,Extraterrestrial Environment ,Computer science ,Astronomy ,Origin of Life ,Bayesian probability ,Bayesian analysis ,FOS: Physical sciences ,Planets ,Astrobiology ,star ,Abiogenesis ,Planet ,Exobiology ,milky-way ,Earth and Planetary Astrophysics (astro-ph.EP) ,Multidisciplinary ,Settore FIS/05 ,Spectrum Analysis ,Bayes Theorem ,Galaxies ,Galaxy ,Biological materials ,Exoplanet ,exoplanets ,Extraterrestrial life ,Panspermia ,Physical Sciences ,biosignatures ,Astrophysics - Earth and Planetary Astrophysics - Abstract
One of the major goals for astronomy in the next decades is the remote search for biosignatures (i.e.\ the spectroscopic evidence of biological activity) in exoplanets. Here, we adopt a Bayesian statistical framework to discuss the implications of such future searches, both in the case when life is detected, and when no definite evidence is found. We show that even a single detection of biosignatures in the vicinity of our stellar system, in a survey of similar size to what will be obtainable in the next two decades, would affect significantly our prior belief on the frequency of life in the universe, even starting from a neutral or pessimistic stance. In particular, after such discovery, an initially agnostic observer would be led to conclude that there are more than $10^5$ inhabited planets in the galaxy with a probability exceeding $95$\%. However, this conclusion would be somewhat weakened by the viability of transfer of biological material over interstellar distances, as in panspermia scenarios. Conversely, the lack of significant evidence of biosignatures would have little effect, leaving the assessment of the abundance of life in the galaxy still largely undetermined., Comment: Published on PNAS
- Published
- 2020
21. The southern stellar stream spectroscopic survey (S5)
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Lara R. Cullinane, A. K. Vivas, E. Balbinot, Vasily Belokurov, Daniel B. Zucker, Sergey E. Koposov, Jeffrey D. Simpson, Sanjib Sharma, Alasdair Mackey, Denis Erkal, G. M. De Silva, Douglas L. Tucker, Risa H. Wechsler, J. D. Simon, Keith Bechtol, Kyler Kuehn, Alexander P. Ji, Geraint F. Lewis, Alex Drlica-Wagner, Brian Yanny, Marla Geha, Joss Bland-Hawthorn, Andrew B. Pace, S. Allam, Nora Shipp, G. S. Da Costa, Tenglin Li, Andrew R. Casey, Jeremy Mould, Zhen Wan, Yao-Yuan Mao, Sarah L. Martell, and Astronomy
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TIDAL STREAMS ,Milky Way ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,MASS ,01 natural sciences ,globular clusters: general ,Photometry (optics) ,Galactic halo ,DARK HALO ,galaxy: halo ,0103 physical sciences ,SPECTROGRAPH ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Dwarf galaxy ,media_common ,Physics ,RADIAL-VELOCITIES ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,galaxies: dwarf ,Astrophysics - Astrophysics of Galaxies ,GIANT STARS ,Galaxy ,EVOLUTION ,GALAXY ,Dark matter halo ,Space and Planetary Science ,Sky ,Globular cluster ,Astrophysics of Galaxies (astro-ph.GA) ,galaxy: kinematics and dynamics ,DIGITAL SKY SURVEY ,MILKY-WAY ,Astrophysics::Earth and Planetary Astrophysics - Abstract
We introduce the Southern Stellar Stream Spectroscopy Survey (${S}^5$), an on-going program to map the kinematics and chemistry of stellar streams in the Southern Hemisphere. The initial focus of ${S}^5$ has been spectroscopic observations of recently identified streams within the footprint of the Dark Energy Survey (DES), with the eventual goal of surveying streams across the entire southern sky. Stellar streams are composed of material that has been tidally striped from dwarf galaxies and globular clusters and hence are excellent dynamical probes of the gravitational potential of the Milky Way, as well as providing a detailed snapshot of its accretion history. Observing with the 3.9-m Anglo-Australian Telescope's 2-degree-Field fibre positioner and AAOmega spectrograph, and combining the precise photometry of DES DR1 with the superb proper motions from $Gaia$ DR2, allows us to conduct an efficient spectroscopic survey to map these stellar streams. So far ${S}^5$ has mapped 9 DES streams and 3 streams outside of DES; the former are the first spectroscopic observations of these recently discovered streams. In addition to the stream survey, we use spare fibres to undertake a Milky Way halo survey and a low-redshift galaxy survey. This paper presents an overview of the ${S}^5$ program, describing the scientific motivation for the survey, target selection, observation strategy, data reduction and survey validation. Finally, we describe early science results on stellar streams and Milky Way halo stars drawn from the survey. Updates on ${S}^5$, including future public data release, can be found at \url{http://s5collab.github.io}., Comment: 25 pages, 14 figures (1 in appendix), 3 tables (1 in appendix). Published on MNRAS. See also paper from Shipp et al. 2019, which measures the proper motion of the DES streams
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- 2019
22. PHANGS-JWST First Results: Spurring on Star Formation: JWST Reveals Localized Star Formation in a Spiral Arm Spur of NGC 628
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Thomas G. Williams, Jiayi Sun, Ashley T. Barnes, Eva Schinnerer, Jonathan D. Henshaw, Sharon E. Meidt, Miguel Querejeta, Elizabeth J. Watkins, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Mélanie Chevance, Oleg V. Egorov, Eric Emsellem, Simon C. O. Glover, Kathryn Grasha, Hamid Hassani, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Ismael Pessa, Jérôme Pety, Francesca Pinna, Erik Rosolowsky, Karin M. Sandstrom, Rowan Smith, Mattia C. Sormani, Sophia Stuber, David A. Thilker, and Bradley C. Whitmore
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INTERSTELLAR-MEDIUM ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,MOLECULAR GAS ,EVOLUTION ,SIMULATIONS ,GALAXIES ,ASTROPY ,Physics and Astronomy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,MILKY-WAY ,CLOUD-CLOUD COLLISIONS ,HIGH-RESOLUTION - Abstract
We combine JWST observations with ALMA CO and VLT-MUSE H$\alpha$ data to examine off-spiral arm star formation in the face-on, grand-design spiral galaxy NGC 628. We focus on the northern spiral arm, around a galactocentric radius of 3-4 kpc, and study two spurs. These form an interesting contrast, as one is CO-rich and one CO-poor, and they have a maximum azimuthal offset in MIRI 21$\mu$m and MUSE H$\alpha$ of around 40$^\circ$ (CO-rich) and 55$^\circ$ (CO-poor) from the spiral arm. The star formation rate is higher in the regions of the spurs near to spiral arms, but the star formation efficiency appears relatively constant. Given the spiral pattern speed and rotation curve of this galaxy and assuming material exiting the arms undergoes purely circular motion, these offsets would be reached in 100-150 Myr, significantly longer than the 21$\mu$m and H$\alpha$ star formation timescales (both, Comment: 11 pages, 5 Figures, accepted as part of a PHANGS-JWST Focus Issue to appear in ApJ. Updated to include missing author and published paper references
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- 2022
23. Gravitational waves as a probe of globular cluster formation and evolution
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Eric Thrane, Johan Samsing, I. M. Romero-Shaw, Kyle Kremer, and Paul D. Lasky
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first stars ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Compact star ,MASS ,01 natural sciences ,STAR-FORMATION ,0103 physical sciences ,Cluster (physics) ,black holes [stars] ,Astrophysics::Solar and Stellar Astrophysics ,dark ages ,010306 general physics ,010303 astronomy & astrophysics ,Reionization ,Astrophysics::Galaxy Astrophysics ,general [globular clusters] ,black hole mergers ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,BILBY ,Gravitational wave ,METAL-RICH ,Order (ring theory) ,Astronomy and Astrophysics ,PERTURBATIONS ,Redshift ,gravitational waves ,Space and Planetary Science ,Globular cluster ,Dark Ages ,reionization ,MILKY-WAY ,star formation [galaxies] ,Astrophysics - High Energy Astrophysical Phenomena ,BAYESIAN-INFERENCE ,MONTE-CARLO SIMULATIONS ,BINARY STARS ,BLACK-HOLE MERGERS - Abstract
Globular clusters are considered to be likely breeding grounds for compact binary mergers. In this paper, we demonstrate how the gravitational-wave signals produced by compact object mergers can act as tracers of globular cluster formation and evolution. Globular cluster formation is a long-standing mystery in astrophysics, with multiple competing theories describing when and how globular clusters formed. The limited sensitivity of electromagnetic telescopes inhibits our ability to directly observe globular cluster formation. However, with future audio-band detectors sensitive out to redshifts of z ≈ 50 for GW150914-like signals, gravitational-wave astronomy will enable us to probe the Universe when the first globular clusters formed. We simulate a population of binary black hole mergers from theoretically motivated globular cluster formation models, and construct redshift measurements consistent with the predicted accuracy of third-generation detectors. We show that we can locate the peak time of a cluster formation epoch during reionization to within 0.05 Gyr after 1 yr of observations. The peak of a formation epoch that coincides with the Universal star formation rate can be measured to within 0.4–10.5 Gyr after 1 yr of observations, depending on the relative weighting of the model components.
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- 2021
24. A census of young stellar objects in two line-of-sight star-forming regions toward IRAS 22147+5948 in the outer Galaxy
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Agata Karska, Maciej Koprowski, Aleksandra Solarz, Ryszard Szczerba, Marta Sewiło, Natasza Siódmiak, Davide Elia, Marcin Gawroński, Konrad Grzesiak, Bosco H. K. Yung, William J. Fischer, and Lars E. Kristensen
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formation [stars] ,PARSEC EVOLUTIONARY TRACKS ,LEGACY ,FOS: Physical sciences ,PROTOSTARS ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,SOLAR CIRCLE ,Astrophysics - Astrophysics of Galaxies ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,MOLECULAR CLOUDS ,Astrophysics::Solar and Stellar Astrophysics ,MILKY-WAY ,individual objects: IRAS 22147+5948 [ISM] ,Astrophysics::Earth and Planetary Astrophysics ,EMISSION ,HERSCHEL-PACS ,Astrophysics::Galaxy Astrophysics ,molecules [ISM] ,MASSIVE STARS ,GALACTIC-PLANE SURVEY - Abstract
(abridged) Star formation in the outer Galaxy, i.e., outside of the Solar circle, has been lightly studied in part due to low CO brightness of molecular clouds linked with the negative metallicity gradient. Recent infrared surveys provide an overview of dust emission in large sections of the Galaxy, but suffer from cloud confusion and poor spatial resolution at far-infrared wavelengths. We aim to develop a methodology to identify and classify young stellar objects (YSOs) in star-forming regions in the outer Galaxy, and use it to solve a long-standing confusion with the distance and evolutionary status of IRAS 22147+5948. We use Support Vector Machine learning algorithm to complement standard color-color and color-magnitude diagrams in search for YSOs in the IRAS 22147 region using publicly available data from the `Spitzer Mapping of the Outer Galaxy' survey. The agglomerative hierarchical clustering algorithm is used to identify clusters, along with the Robitaille et al. (2017) code to calculate physical properties of individual YSOs. We identify 13 Class I and 13 Class II YSO candidates using the color-color diagrams, and additional 2 and 21 sources, respectively, using the machine learning techniques. Spectral energy distributions of 23 sources are modelled with a star and a passive disk, corresponding to Class II objects. Models of 3 sources include envelopes typical for Class I objects. The objects are grouped in 2 clusters located at the distance of ~2.2 kpc, and 5 clusters at ~5.6 kpc. The spatial extent of CO, radio continuum, and dust emission confirms the origin of YSOs in two distinct star-forming regions along a similar line-of-sight. The outer Galaxy might serve as a unique laboratory of star formation across environments on condition that complementary methods and ancillary data are used to properly account for cloud confusion and distance uncertainties., 29 pages, 17 figures, 9 tables
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- 2022
25. Weighing the Galactic disk using phase-space spirals
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Axel Widmark, Jason Hunt, Chervin Laporte, Giacomo Monari, Carlsberg Foundation, European Research Council, European Commission, Flatiron Institute, Agence Nationale de la Recherche (France), and Villum Fonden
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Solar neighborhood ,solar neighborhood ,kinematics and dynamics ,disk ,FOS: Physical sciences ,BULGE-HALO MODELS ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrometry ,Astrophysics - Astrophysics of Galaxies ,Galaxy: disk ,Galaxy ,SAGITTARIUS ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,astrometry ,MILKY-WAY ,Galaxy: kinematics and dynamics ,Astrophysics::Galaxy Astrophysics - Abstract
In this fourth article on weighing the Galactic disk using the shape of the phase-space spiral, we have tested our method on a billion particle three-dimensional N-body simulation, comprised of a Milky Way like host galaxy and a merging dwarf satellite. The main purpose of this work was to test the validity of our model’s fundamental assumptions that the spiral inhabits a locally static and vertically separable gravitational potential. These assumptions might be compromised in the complex kinematic system of a disturbed three-dimensional disk galaxy; in fact, the statistical uncertainty and any potential biases related to these assumptions are expected to be amplified for this simulation, which differs from the Milky Way in that it is more strongly perturbed and has a phase-space spiral that inhabits higher vertical energies. We constructed 44 separate data samples from different spatial locations in the simulated host galaxy. Our method produced accurate results for the vertical gravitational potential of these 44 data samples, with an unbiased distribution of errors with a standard deviation of 7%. We also tested our method under severe and unknown spatially dependent selection effects, also with robust results; this sets it apart from traditional dynamical mass measurements that are based on the assumption of a steady state and which are highly sensitive to unknown or poorly modelled incompleteness. Hence, we will be able to make localised mass measurements of distant regions in the Milky Way disk, which would otherwise be compromised by complex and poorly understood selection effects., AW acknowledges support from the Carlsberg Foundation via a Semper Ardens grant (CF15-0384). JH is supported by a Flatiron Research Fellowship at the Flatiron institute, which is supported by the Simons Foundation. CL acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 852839). GM acknowledges funding from the Agence Nationale de la Recherche (ANR project ANR-18-CE31-0006 and ANR-19-CE31-0017) and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 834148). This work made use of an HPC facility funded by a grant from VILLUM FONDEN (projectnumber 16599). This research utilised the following open-source Python packages: MATPLOTLIB (Hunter 2007), NUMPY (Harris et al. 2020), SCIPY (Virtanen et al. 2020), PANDAS (McKinney et al. 2010), TENSORFLOW (Abadi et al. 2015).
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- 2022
26. The tidal remnant of an unusually metal-poor globular cluster
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Jeffrey D. Simpson, Geraint F. Lewis, Zhen Wan, Eduardo Balbinot, Daniel B. Zucker, Prajwal R. Kafle, Gayandhi M. De Silva, Nora Shipp, Dougal Mackey, Alexander P. Ji, Joss Bland-Hawthorn, Sanjib Sharma, Andrew R. Casey, Andrew B. Pace, Ting S. Li, Sarah L. Martell, Kyler Kuehn, Jeremy Mould, Sergey E. Koposov, Denis Erkal, Gary S. Da Costa, and Astronomy
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II ,Metallicity ,media_common.quotation_subject ,Milky Way ,astro-ph.GA ,Population ,FOS: Physical sciences ,EFFICIENT ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,MASS ,01 natural sciences ,GAPS ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,STREAMS ,education ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,Physics ,education.field_of_study ,Multidisciplinary ,010308 nuclear & particles physics ,METALLICITY INDICATOR ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,Universe ,GALAXY ,Globular cluster ,Astrophysics of Galaxies (astro-ph.GA) ,MILKY-WAY ,TRIPLET ,Halo ,Astrophysics::Earth and Planetary Astrophysics - Abstract
Globular clusters are some of the oldest bound stellar structures observed in the Universe. They are ubiquitous in large galaxies and are believed to trace intense star formation events and the hierarchical build-up of structure. Observations of globular clusters in the Milky Way, and a wide variety of other galaxies, have found evidence for a `metallicity floor', whereby no globular clusters are found with chemical (`metal') abundances below approximately 0.3 to 0.4 per cent of that of the Sun. The existence of this metallicity floor may reflect a minimum mass and a maximum redshift for surviving globular clusters to form, both critical components for understanding the build-up of mass in the universe. Here we report measurements from the Southern Stellar Streams Spectroscopic Survey of the spatially thin, dynamically cold Phoenix stellar stream in the halo of the Milky Way. The properties of the Phoenix stream are consistent with it being the tidally disrupted remains of a globular cluster. However, its metal abundance ([Fe/H] = -2.7) is substantially below that of the empirical metallicity floor. The Phoenix stream thus represents the debris of the most metal-poor globular cluster discovered so far, and its progenitor is distinct from the present-day globular cluster population in the local Universe. Its existence implies that globular clusters below the metallicity floor have probably existed, but were destroyed during Galactic evolution., Comment: Authors' version of an Article published in Nature on July 29th, 2020
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- 2020
27. A CO isotopologue Line Atlas within the Whirlpool galaxy Survey (CLAWS)
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Jakob S. den Brok, Frank Bigiel, Kazimierz Sliwa, Toshiki Saito, Antonio Usero, Eva Schinnerer, Adam K. Leroy, María J. Jiménez-Donaire, Erik Rosolowsky, Ashley T. Barnes, Johannes Puschnig, Jérôme Pety, Andreas Schruba, Ivana Bešlić, Yixian Cao, Cosima Eibensteiner, Simon C. O. Glover, Ralf S. Klessen, J. M. Diederik Kruijssen, Sharon E. Meidt, Lukas Neumann, Neven Tomičić, Hsi-An Pan, Miguel Querejeta, Elizabeth Watkins, Thomas G. Williams, and David Wilner
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LEGACY SURVEY ,J=2-1 SURVEY ,ISM [galaxies] ,INTERSTELLAR-MEDIUM ,FOS: Physical sciences ,Astronomy and Astrophysics ,CONVERSION FACTOR ,Astrophysics - Astrophysics of Galaxies ,STAR-FORMATION EFFICIENCY ,galaxies [radio lines] ,DENSE MOLECULAR GAS ,Physics and Astronomy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,MILKY-WAY ,NEARBY GALAXIES ,X-FACTOR ,SPIRAL-ARM ,molecules [ISM] - Abstract
We present the CO isotopologue Line Atlas within the Whirpool galaxy Survey (CLAWS) based on an IRAM 30-m large programme which provides a benchmark study of numerous, faint CO isotopologues in the mm-wavelength regime across the full disc of M51 (NGC 5194). The survey's core goal is to use the low-J CO isotopologue lines to constrain CO excitation and chemistry, and therefrom the local physical conditions of the gas. In this survey paper, we describe the CLAWS observing and data reduction strategies. We map the J=1-0 and 2-1 transitions of the CO isotopologues $^{12}$CO,$^{13}$CO, C$^{18}$O and C$^{17}$O, as well as several supplementary lines within the 1 mm and 3 mm window (CN(1-0), CS(2-1), CH$_3$OH(2-1), N$_2$H$^+$(1-0), HC$_3$N(10-9)) at ~1 kpc resolution. A total observation time of 149 h offers unprecedented sensitivity. We use these data to explore several CO isotopologue line ratios in detail, study their radial (and azimuthal) trends and investigate whether changes in line ratios stem from changes in ISM properties such as gas temperatures, densities or chemical abundances. For example, we find negative radial trends for the $^{13}$CO}/$^{12}$CO, C$^{18}$O/$^{12}$CO and C$^{18}$O/$^{13}$CO line ratios in their J=1-0 transitions. We also find variations with local environment, such as higher $^{12}$CO(2-1)/(1-0) or $^{13}$CO/$^{12}$CO(1-0) line ratios in interarm regions compared to spiral arm regions. We propose that these aforementioned variations of CO line ratios are most likely due to a variation of the optical depth, while abundance variations due to selective nucleosynthesis on a galaxy-wide scale could also play a role. We also study the CO spectral line energy distribution (SLED) using archival JCMT $^{12}$CO(3-2) data and find a variation of the SLED shape with local environmental parameters further underlying changes in optical depth, gas temperatures or densities., 29 pages, 22 figures, accepted for publication in A&A
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- 2022
28. The Complexity of the Cetus Stream Unveiled from the Fusion of STREAMFINDER and StarGO
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Zhen Yuan, Khyati Malhan, Federico Sestito, Rodrigo A. Ibata, Nicolas F. Martin, Jiang Chang, Ting S. Li, Elisabetta Caffau, Piercarlo Bonifacio, Michele Bellazzini, Yang Huang, Karina Voggel, Nicolas Longeard, Anke Arentsen, Amandine Doliva-Dolinsky, Julio Navarro, Benoit Famaey, Else Starkenburg, David S. Aguado, and Astronomy
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omega-centauri ,globular-cluster ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,stellar streams ,digital sky survey ,metal-poor stars ,chemical abundances ,sagittarius dwarf galaxy ,milky-way ,spectroscopic survey ,scaling relations - Abstract
We combine the power of two stream-searching tools, STREAMFINDER and StarGO applied to the Gaia EDR3 data, to detect stellar debris belonging to the Cetus stream system that forms a complex, nearly polar structure around the Milky Way. In this work, we find the southern extensions of the northern Cetus stream as the Palca stream and a new southern stream, which overlap on the sky but have different distances. These two stream wraps extend over more than $\sim100\deg$ on the sky ($-60\deg, Comment: accepted to ApJ. The N-body model of the Cetus system is published at https://zenodo.org/record/5771585
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- 2021
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29. The Galactic Anticentre
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Vincenzo Ripepi, A. de Torres, Annie C. Robin, Mariateresa Crosta, C. Diener, L. Noval, Daniel Michalik, P. J. Richards, L. Karbevska, K. Kruszyńska, E. Fraile, André Moitinho, Michał Pawlak, P. Panuzzo, M. Riello, Benoit Carry, A. Yoldas, Harry Enke, N. Tonello, P. Gavras, M. Vaillant, Rosanna Sordo, E. del Pozo, Lorenzo Rimoldini, M. Bernet, G. Orrù, W. van Reeven, J. M. Martín-Fleitas, S. Diakite, P. Burgess, P. Osborne, Derek W. Morris, M. I. Carnerero, Amina Helmi, Mike Smith, Iain A. Steele, Alessandro Sozzetti, M. Kontizas, A. Sagristà Sellés, Roberto Molinaro, B. Holl, D. Baines, D. Molina, J. Fernández-Hernández, S. Marinoni, Michele Bellazzini, Maria Süveges, Teresa Antoja, D. Barbato, Uwe Lammers, Isabella Pagano, Davide Massari, G. Plum, P. Ramos, G. Jevardat de Fombelle, M. Biermann, C. Crowley, Mathias Schultheis, D. W. Evans, P. A. Palicio, Paolo Montegriffo, Ramachrisna Teixeira, R. Blomme, Elmé Breedt, T. A. Lister, F. A. Jansen, Ruth Carballo, Marcella Marconi, A. Abreu Aramburu, J. M. Carrasco, F. Royer, S. Accart, A. Burlacu, S. Regibo, Andrej Prsa, M. Sarasso, Nicolas Rambaux, A. F. Mulone, Ana Ulla, Eric Gosset, Alessandra Mastrobuono-Battisti, George M. Seabroke, H. E. Delgado, Federico Marocco, C. Nicolas, T. Lebzelter, Nami Mowlavi, C. Barache, Nicoletta Sanna, G. Gracia-Abril, R. Santoveña, R. Haigron, N. Unger, Silvio Leccia, A. Jean-Antoine Piccolo, A. F. Lanza, Alberto Vecchiato, Thomas Wevers, F. Figueras, G. Busso, C. Fabre, P. Di Matteo, F. Riclet, F. Solitro, Eric Slezak, N. Samaras, João Alves, Emese Plachy, Timo Prusti, F. van Leeuwen, J. Osinde, O. Marchal, M. Ajaj, C. Ducourant, Tatiana Muraveva, Shay Zucker, H. Steidelmüller, Alberto Riva, D. Semeux, N. Cheek, Laurent Galluccio, Martin A. Barstow, Alex Bombrun, S. Liao, M. van Leeuwen, R. E. de Souza, P. de Laverny, T. Roegiers, Paul J. McMillan, G. Holland, Alexey Mints, G. Giuffrida, L. M. Sarro, Juan Zorec, G. Sadowski, P. Yvard, Carme Jordi, J. L. Halbwachs, Laurent Chemin, Ludovic Delchambre, M. Garcia-Reinaldos, Ugo Becciani, Diego Bossini, Ángel Gómez, Sergi Blanco-Cuaresma, Rossella Cancelliere, C. Fabricius, J. De Ridder, L. Eyer, L. Pulone, Simon Hodgkin, Ennio Poretti, F. De Angeli, M. Haywood, E. Anglada Varela, Antonella Vallenari, F. X. Pineau, D. Garabato, A. Guerrier, H. E. P. Lindstrøm, Thomas Hilger, I. Bellas-Velidis, Frédéric Arenou, Paolo Giacobbe, Ilaria Musella, Tristan Cantat-Gaudin, L. Palaversa, Pedro García-Lario, David Hobbs, C. Turon, E. Balbinot, P. de Teodoro, Sébastien Lambert, D. Katz, Angela Bragaglia, Anthony G. A. Brown, Paolo Tanga, P. Castro Sampol, J. C. Segovia, Alejandra Recio-Blanco, Yves Fremat, Jon Marchant, Jose M Hernandez, S. Ragaini, Sofia Randich, P. Re Fiorentin, J. F. Le Campion, Gisella Clementini, M. Segol, P. David, R. Drimmel, F. Crifo, J. Guiraud, M. David, R. L. Smart, M. Fabrizio, I. Gonzalez-Santamaria, D. Eappachen, M. G. Lattanzi, Miguel García-Torres, Andreas Korn, S. Voutsinas, László Molnár, Simchon Faigler, A. Mora, Nicholas Rowell, Antti Penttilä, R. Geyer, Sanjeev Khanna, Aldo Dell'Oro, H. E. Huckle, C. Dolding, N. Leclerc, Monica Rainer, R. Mor, J. Bakker, Maroussia Roelens, Douglas J. Marshall, A. G. Butkevich, Nigel Hambly, A. Masip, Laia Casamiquela, R. Messineo, Martin Altmann, A. M. Piersimoni, Alessandro Spagna, Gerry Gilmore, Stefano Bertone, Patrick Charlot, O. Vanel, Daniel Hestroffer, Marco Castellani, Sebastian L. Hidalgo, W. Roux, Łukasz Wyrzykowski, Krzysztof A. Rybicki, M. M. S. Marcos Santos, Raphael Guerra, Alberto Cellino, E. Poggio, Gérard Jasniewicz, J. J. González-Vidal, S. Cowell, Peter G. Jonker, C. M. Raiteri, S. Bartolomé, J. Álvarez Cid-Fuentes, Elisabetta Caffau, J. J. Aguado, N. R. Millar, Ulrike Heiter, Federica Spoto, Felix Franke, A. Baudesson-Stella, M. Barros, Tsevi Mazeh, A. Panahi, E. Brugaletta, R. Buzzi, Elena Pancino, G. Altavilla, E. Racero, Enrique Solano, Mikael Granvik, Minia Manteiga, C. Robin, Tomaz Zwitter, Deborah Busonero, Alberto Krone-Martins, Marc Audard, Kevin Benson, Christos Siopis, L. Balaguer-Núñez, C. A. L. Bailer-Jones, E. Poujoulet, O. L. Creevey, E. Szegedi-Elek, C. Fouron, Michael Davidson, E. Licata, Despina Hatzidimitriou, Mark Cropper, Z. Kostrzewa-Rutkowska, S. Managau, A. Dapergolas, Sergio Messina, Laszlo Szabados, H. I. Siddiqui, W. Löffler, Mario Gai, J.-B. Delisle, Leanne P. Guy, S. G. Baker, W. J. Cooper, Alfred Castro-Ginard, Conny Aerts, A. Lorca, Xavier Luri, Damien Ségransan, Grigori Fedorets, A. Garofalo, J. Juaristi Campillo, F. De Luise, F. Pailler, F. Taris, L. Bramante, Thierry Morel, T. Cornez, L. Martin Polo, M. Ramos-Lerate, Jordi Portell, E. Salguero, Sergei A. Klioner, K. Janßen, Ulrich Bastian, Stefan Jordan, P. Esquej, A. C. Lanzafame, Beatrice Bucciarelli, C. Panem, Y. Lebreton, Carlos Dafonte, S. Girona, D. Munoz, Dimitri Pourbaix, William Thuillot, J. H. J. de Bruijne, N. Brouillet, L. Chaoul, F. Torra, Alex Lobel, J.-L. Bassilana, Francesca Fragkoudi, M. Romero-Gómez, C. A. Stephenson, T. Pauwels, Eva Sciacca, Alessandro Bressan, Morgan Fouesneau, E. Livanou, E. Gerlach, X. Peñalosa Esteller, Roberto Morbidelli, L. Rohrbasser, Johannes Sahlmann, Elisa Distefano, P. Sartoretti, Karri Muinonen, Zoltan Balog, Y. Viala, J. Torra, H. Zhao, L. Siltala, G. Tauran, D. Souami, P. Madrero Pardo, David Teyssier, Jesus Salgado, J. Souchay, C. P. Murphy, Maria-Rosa L. Cioni, N. A. Walton, S. Bouquillon, Andrea Chiavassa, Agnes Fienga, Giovanni Comoretto, F. Julbe, A. Hutton, Yassine Damerdji, Richard I. Anderson, Pierre Fernique, Céline Reylé, M. Hauser, E. Utrilla, Pierre Kervella, C. Zurbach, Robert G. Mann, Ummi Abbas, Hector Canovas, D. L. Harrison, Y. Lasne, Mark Taylor, Y. Le Fustec, E. F. del Peloso, N. Bauchet, E. van Dillen, Jan Rybizki, N. Hładczuk, T. Boch, J. González-Núñez, Carine Babusiaux, C. Pagani, Krzysztof Nienartowicz, Eduard Masana, G. Kordopatis, N. Robichon, Luciana Bianchi, R. Gutiérrez-Sánchez, Arnaud Siebert, A. Kochoska, T. Carlucci, Jérôme Berthier, J. Castañeda, D. Vicente, R. De March, A. Garcia-Gutierrez, M. Weiler, F. Thévenin, Lennart Lindegren, Isabelle Lecoeur-Taïbi, Guy Rixon, Francois Mignard, P. M. Marrese, M. A. Álvarez, Caroline Soubiran, Rene Andrae, C. Ordénovic, A. Delgado, V. Sanchez Gimenez, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Universidad de Barcelona, Xunta de Galicia, European Commission, Centros de Excelencia Severo Ochoa, BARCELONA SUPERCOMPUTING CENTER (BSC), SEV2015-0493, Krone Martins, A. [0000-0002-2308-6623], McMillan, P. [0000-0002-8861-2620], Carrasco Martínez, J. P. [0000-0002-3029-5853], Sozzetti, A. [0000-0002-7504-365X], Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MINECO/ICTI2013-2016/MDM-2014-0369, Centrode Excelencia Científica Instituto de Ciencias del Cosmos Universidad de Barcelona, MINECO/ICTI2013-2016/SEV2015-0493, Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES), National Natural Science Foundation of China (NSFC), Estonian Ministry of Education and Research, Centre National D'Etudes Spatiales (CNES), Agence Nationale de la Recherche (ANR), Centre National de la Recherche Scientifique (CNRS), European Commission (EC), European Research Council (ERC), Institut des Sciences de l'Univers (INSU), Institut National Polytechnique (INP), Institut National de Physique nucleaire et de Physique des Particules (IN2P3), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Hungarian Academy of Sciences, Hungarian National Research, Development, and Innovation Office (NKFIH), Science Foundation Ireland (SFI), Israel Science Foundation (ISF), Agenzia Spaziale Italiana (ASI), Italian Istituto Nazionale di Astrofisica (INAF), Netherlands Organisation for Scientific Research (NWO), Polish National Science Centre, Ministry of Science and Higher Education (MNiSW), Fundacao para a Ciencia e a Tecnologia (FCT), Slovenian Research Agency, Agencia Estatal de Investigación (AEI), Generalitat de Catalunya, United Kingdom Science and Technology Facilities Council (STFC), United Kingdom Space Agency (UKSA), Gaia Collaboration, Universidad de Cantabria, Astronomy, Kapteyn Astronomical Institute, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), M2A 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Planetary-system research, Department of Physics, Particle Physics and Astrophysics, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
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trigonometric parallaxes ,SOLAR NEIGHBORHOOD ,Astronomy ,SAGITTARIUS DWARF GALAXY ,Astrophysics ,01 natural sciences ,sagittarius dwarf galaxy ,010303 astronomy & astrophysics ,Physics ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,solar neighborhood ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrometry ,Gelexy: kinematics and dynamics ,Kinematics and Dynamics ,Open clusters and asssociations: individual: Berkeley 29 ,sky survey ,Disk ,Physical Sciences ,kinematics and dynamics [Gelexy] ,old open clusters ,MILKY-WAY ,Astrophysics::Earth and Planetary Astrophysics ,open clusters and associations: individual: Berkeley 29 ,Galaxy: kinematics and dynamics ,disk [Galaxy] ,individual: Berkeley 29 [open clusters and associations] ,Astrometria ,Berkeley 29 ,EXPLORING HALO SUBSTRUCTURE ,LOCAL KINEMATICS ,Milky Way ,FOS: Physical sciences ,Open Clusters and Associations ,Individual ,exploring halo substructure ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Computer Science::Digital Libraries ,stellar structure ,Galaxy: disk ,Open clusters and associations: individual: Saurer 1 ,Galactic halo ,Halo ,Settore FIS/05 - Astronomia e Astrofisica ,individual: Berkeley 29 [Open clusters and asssociations] ,0103 physical sciences ,distances [stars] ,halo [Galaxy] ,Disc ,Stars: distances ,milky-way ,Saurer 1 ,Astrophysics::Galaxy Astrophysics ,canis-major ,Science & Technology ,010308 nuclear & particles physics ,TRIGONOMETRIC PARALLAXES ,Galaxy: halo ,stars: distances ,open clusters and associations: individual: Saurer 1 ,Astrophysics - Astrophysics of Galaxies ,Astronomy and Astrophysics ,Galactic plane ,kinematics and dynamics [Galaxy] ,115 Astronomy, Space science ,CANIS-MAJOR ,Stars ,Galaxy ,Physics::History of Physics ,Estels ,individual: Saurer 1 [open clusters and associations] ,Distances ,local kinematics ,OLD OPEN CLUSTERS ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,SKY SURVEY ,Open cluster ,STELLAR STRUCTURE - Abstract
Aims. We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of different aspects of the Milky Way structure and evolution and we provide, at the same time, a description of several practical aspects of the data and examples of their usage., Methods. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. In this direction, the Gaia astrometric data alone enable the calculation of the vertical and azimuthal velocities; also, the extinction is relatively low compared to other directions in the Galactic plane. We then explore the disturbances of the current disc, the spatial and kinematical distributions of early accreted versus in situ stars, the structures in the outer parts of the disc, and the orbits of open clusters Berkeley 29 and Saurer 1., Results. With the improved astrometry and photometry of EDR3, we find that: (i) the dynamics of the Galactic disc are very complex with oscillations in the median rotation and vertical velocities as a function of radius, vertical asymmetries, and new correlations, including a bimodality with disc stars with large angular momentum moving vertically upwards from below the plane, and disc stars with slightly lower angular momentum moving preferentially downwards; (ii) we resolve the kinematic substructure (diagonal ridges) in the outer parts of the disc for the first time; (iii) the red sequence that has been associated with the proto-Galactic disc that was present at the time of the merger with Gaia-Enceladus-Sausage is currently radially concentrated up to around 14 kpc, while the blue sequence that has been associated with debris of the satellite extends beyond that; (iv) there are density structures in the outer disc, both above and below the plane, most probably related to Monoceros, the Anticentre Stream, and TriAnd, for which the Gaia data allow an exhaustive selection of candidate member stars and dynamical study; and (v) the open clusters Berkeley 29 and Saurer 1, despite being located at large distances from the Galactic centre, are on nearly circular disc-like orbits., Conclusions. Even with our simple preliminary exploration of the Gaia EDR3, we demonstrate how, once again, these data from the European Space Agency are crucial for our understanding of the different pieces of our Galaxy and their connection to its global structure and history.
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30. Dense molecular gas properties on 100 pc scales across the disc of NGC 3627
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Mattia C. Sormani, Daizhong Liu, Annie Hughes, Andreas Schruba, Christopher M Faesi, M. J. Jimenez-Donaire, Takashi Saito, J. M. D. Kruijssen, Francesco Belfiore, Frank Bigiel, Eric Emsellem, Ismael Pessa, Ralf S. Klessen, Simon C. O. Glover, Jérôme Pety, Ashley T. Barnes, Mélanie Chevance, Sharon Meidt, Eva Schinnerer, Ivana Bešlić, Thomas G. Williams, Kathryn Kreckel, F. Santoro, C. Herrera Contreras, A. Usero, Cosima Eibensteiner, Kathryn Grasha, J. Puschnig, Adam K. Leroy, M. Querejeta, J. S. den Brok, Erik Rosolowsky, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
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H-ALPHA ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,STAR-FORMATION RATES ,BIMA SURVEY ,ISM STRUCTURE ,01 natural sciences ,ISM: clouds ,0103 physical sciences ,LINE SPECTRA ,NEARBY GALAXIES ,Emission spectrum ,010303 astronomy & astrophysics ,molecules [ISM] ,evolution [galaxies] ,Astrophysics::Galaxy Astrophysics ,Physics ,[PHYS]Physics [physics] ,Spiral galaxy ,formation [stars] ,stars: formation ,ISM [galaxies] ,010308 nuclear & particles physics ,Star formation ,Astronomy and Astrophysics ,Radius ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,ISM: molecules ,Interstellar medium ,Barred spiral galaxy ,Stars ,Physics and Astronomy ,13. Climate action ,Space and Planetary Science ,galaxies: star formation ,Astrophysics of Galaxies (astro-ph.GA) ,COMPUTER-PROGRAM ,MILKY-WAY ,Astrophysics::Earth and Planetary Astrophysics ,star formation [galaxies] ,galaxies: evolution ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,clouds [ISM] ,UNCERTAINTY PRINCIPLE ,galaxies: ISM ,GALACTIC-CENTER - Abstract
It is still poorly constrained how the densest phase of the interstellar medium varies across galactic environment. A large observing time is required to recover significant emission from dense molecular gas at high spatial resolution, and to cover a large dynamic range of extragalactic disc environments. We present new NOrthern Extended Millimeter Array (NOEMA) observations of a range of high critical density molecular tracers (HCN, HNC, HCO+) and CO isotopologues (13CO, C18O) towards the nearby (11.3 Mpc), strongly barred galaxy NGC 3627. These observations represent the current highest angular resolution (1.85"; 100 pc) map of dense gas tracers across a disc of a nearby spiral galaxy, which we use here to assess the properties of the dense molecular gas, and their variation as a function of galactocentric radius, molecular gas, and star formation. We find that the HCN(1-0)/CO(2-1) integrated intensity ratio does not correlate with the amount of recent star formation. Instead, the HCN(1-0)/CO(2-1) ratio depends on the galactic environment, with differences between the galaxy centre, bar, and bar end regions. The dense gas in the central 600 pc appears to produce stars less efficiently despite containing a higher fraction of dense molecular gas than the bar ends where the star formation is enhanced. In assessing the dynamics of the dense gas, we find the HCN(1-0) and HCO+(1-0) emission lines showing multiple components towards regions in the bar ends that correspond to previously identified features in CO emission. These features are co-spatial with peaks of Halpha emission, which highlights that the complex dynamics of this bar end region could be linked to local enhancements in the star formation., Comment: 25 pages, 12 figures; accepted for publication in MNRAS
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- 2021
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31. The Pristine survey XIV: chemical analysis of two ultra-metal-poor stars
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Else Starkenburg, Julio F. Navarro, Lyudmila Mashonkina, Collin Kielty, Piercarlo Bonifacio, K. A. Venn, Pascale Jablonka, A. Arentsen, Nicolas F. Martin, Federico Sestito, Tatyana Sitnova, Carmela Lardo, G. Kordopatis, Elisabetta Caffau, J. I. González Hernández, R. G. Carlberg, David Aguado, Vanessa Hill, Università degli Studi di Bologna, Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Instituto de Astrofisica de Canarias (IAC), Universidad de La Laguna [Tenerife - SP] (ULL), University of Victoria [Canada] (UVIC), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l’Université, 67000 Strasbourg, France, Department of Astronomy & Astrophysics [University of Toronto], University of Toronto, Astronomy, Lardo C., Mashonkina L., Jablonka P., Bonifacio P., Caffau E., Aguado D.S., Gonzalez Hernandez J.I., Sestito F., Kielty C.L., Venn K.A., Hill V., Starkenburg E., Martin N.F., Sitnova T., Arentsen A., Carlberg R.G., Navarro J.F., and Kordopatis G.
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stars: abundances ,sodium abundance ,Analytical chemistry ,stellar parameters ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Metal ,Galactic halo ,hamburg/eso survey ,statistical equilibrium ,0103 physical sciences ,Galaxy formation and evolution ,follow-up ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,milky-way ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Physics ,data release ,Galaxy: evolution ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,model atmospheres ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,equilibrium-line formation ,Galaxy: halo ,Galaxy: abundance ,Radial velocity ,Stars ,Supernova ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Galaxy: formation ,visual_art ,Astrophysics of Galaxies (astro-ph.GA) ,visual_art.visual_art_medium ,Galaxy: abundances ,non-lte ,Astrophysics::Earth and Planetary Astrophysics - Abstract
Elemental abundances of the most metal-poor stars reflect the conditions in the early Galaxy and the properties of the first stars. We present a spectroscopic follow-up of two ultra metal-poor stars ([Fe/H], Comment: 17 pages, 11 figures, accepted for publication in MNRAS
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32. Metal-poor stars observed with the automated planet finder telescope. III. CEMP-no stars are the descendant of population III stars
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Maria Rah, Gang Zhao, Nour Aldein Almusleh, Sergen Özdemir, Ali Taani, Mohammad K. Mardini, and Mashhoor A. Al-Wardat
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galaxies structure ,Stellar mass ,Astrophysics::High Energy Astrophysical Phenomena ,Metallicity ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Discovery ,01 natural sciences ,Galactic halo ,Abundance ,Planet ,Fragmentation ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Early Accretion ,In-Situ ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,Cosmic Gas Clouds ,010308 nuclear & particles physics ,abundances ,Astronomy and Astrophysics ,Chemodynamical Analysis ,Astrophysics - Astrophysics of Galaxies ,Milky-Way ,Galaxy ,Accretion (astrophysics) ,Stars ,Supernova ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,stars kinematics and dynamics ,Astrophysics::Earth and Planetary Astrophysics ,Stellar Halo ,halo stars - Abstract
This study reports a probabilistic insight into the stellar-mass and supernovae (SNe) explosion energy of five CEMP-no stars' possible progenitors. As such, a direct comparison between the abundance ratios [X/Fe] of the light-elements and the predicted nucleosynthetic yields of SN of high-mass metal-free stars has been performed. This comparison suggests that the possible progenitors have a stellar-mass range of 11 - 22 M-circle dot and explosion energies of 0.3 - 1.8 x 10(51) erg. In addition, we investigate the kinematic signatures, derived from Gaia DR2, to conclude that these five CEMP-no stars have halo-like kinematic and do not enter the outer-halo region. In addition, we link the abundance patterns with kinematic signatures to investigate the Gaia-Sausage and Gaia-Sequoia memberships. This chemo-dynamical analysis suggests that these CEMP-no stars are neither Gaia-Sausage nor Gaia-Sequoia remnant stars, but another accretion event might be responsible for the contribution of these stars to the Galactic Halo.
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- 2021
33. Weighing the Galactic disk using phase-space spirals I. Tests on one-dimensional simulations
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P. F. de Salas, Axel Widmark, and Chervin F. P. Laporte
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WAVES ,Perturbation (astronomy) ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,MASS MODELS ,Gravitation ,Gravitational potential ,0103 physical sciences ,Vertical direction ,KINEMATICS ,Disc ,010306 general physics ,010303 astronomy & astrophysics ,Spiral ,Astrophysics::Galaxy Astrophysics ,Physics ,Number density ,solar neighborhood ,Computer Science::Information Retrieval ,HUNT ,Astronomy and Astrophysics ,PLANE ,kinematics and dynamics [Galaxy] ,Astrophysics - Astrophysics of Galaxies ,Computational physics ,SAGITTARIUS ,Space and Planetary Science ,DENSITY ,Phase space ,Astrophysics of Galaxies (astro-ph.GA) ,HALO ,astrometry ,MILKY-WAY ,disk [Galaxy] ,STARS - Abstract
We present a new method for inferring the gravitational potential of the Galactic disk, using the time-varying structure of a phase-space spiral in the $(z,w)$-plane (where $z$ and $w$ represent vertical position and vertical velocity). Our method of inference extracts information from the shape of the spiral and disregards the bulk density distribution that is usually used to perform dynamical mass measurements. In this manner, it is complementary to traditional methods that are based on the assumption of a steady state. Our method consists of fitting an analytical model for the phase-space spiral to data, where the spiral is seen as a perturbation of the stellar number density in the $(z,w)$-plane. We tested our method on one-dimensional simulations, which were initiated in a steady state and then perturbed by an external force similar to that of a passing satellite. We were able to retrieve the true gravitational potentials of the simulations with high accuracy. The gravitational potential at 400-500 parsec distances from the disk mid-plane was inferred with an error of only a few percent. This is the first paper of a series in which we plan to test and refine our method on more complex simulations, as well as apply our method to Gaia data., Comment: 16 pages, 12 figures
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- 2021
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34. Metallicity Distribution Function of the Eridanus~II Ultra-Faint Dwarf Galaxy from Hubble Space Telescope Narrow-band Imaging
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Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alexander P. Ji, Ekta Patel, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Nicolas Longeard, Mario L. Mateo, Nathan R. Sandford, and Astronomy
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star-formation ,globular-cluster ,cosmological simulations ,stellar populations ,metal abundances ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,draco ii ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,giant stars ,milky-way ,pristine survey ,spectroscopic confirmation - Abstract
We use deep narrowband Ca H&K ($F395N$) imaging taken with the Hubble Space Telescope (HST) to construct the metallicity distribution function (MDF) of Local Group (LG) ultra-faint dwarf (UFD) galaxy Eridanus II (Eri II). When combined with archival $F475W$ and $F814W$ data, we measure metallicities for 60 resolved red giant branch stars as faint as $m_{F475W}\sim24$ mag, a factor of $\sim4$x more stars than current spectroscopic MDF determinations. We find that Eri II has a mean metallicity of [Fe/H]$=$-2.50$^{+0.07}_{-0.07}$ and a dispersion of $��_{\mbox{[Fe/H]}}=0.42^{+0.06}_{-0.06}$, which are consistent with spectroscopic MDFs, though more precisely constrained owing to a larger sample. We identify a handful of extremely metal-poor star candidates (EMP; [Fe/H] $< -3$) that are marginally bright enough for spectroscopic follow up. Eri II's MDF appears well-described by a leaky box chemical evolution model. We also compute an updated orbital history for Eri II using Gaia eDR3 proper motions, and find that it is likely on first infall into the Milky Way. Our findings suggest that Eri II underwent an evolutionary history similar to that of an isolated galaxy. Compared to MDFs for select cosmological simulations of similar mass galaxies, we find that Eri II has a lower fraction of stars with [Fe/H] $< -3$, though such comparisons should currently be treated with caution due to a paucity of simulations, selection effects, and known limitations of Ca H&K for EMPs. This study demonstrates the power of deep HST CaHK imaging for measuring the MDFs of UFDs., Resubmitted to ApJ with revisions following a positive referee report of the initial draft; 29 pages, 19 figures, and 3 tables, including appendix. Comments welcome!
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35. The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: a multitracer analysis in Fourier space for measuring the cosmic structure growth and expansion rate
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J. Bautista, Jean-Paul Kneib, Jiamin Hou, Arman Shafieloo, Atsushi Taruya, Ashley J. Ross, Chia-Hsun Chuang, Gong-Bo Zhao, Jeffrey A. Newman, V. Ruhlmann-Kleider, Eva Maria Mueller, Kyle S. Dawson, Arnaud de Mattia, John A. Peacock, Cheng Zhao, Etienne Burtin, Will J. Percival, Graziano Rossi, Hélion du Mas des Bourboux, Shadab Alam, Kazuya Koyama, Weibing Zhang, Donald P. Schneider, Anand Raichoor, Yuting Wang, Héctor Gil-Marín, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, National Key Research and Development Program (China), and European Commission
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Particle physics ,Expansion rate ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Structure (category theory) ,FOS: Physical sciences ,Lambda ,01 natural sciences ,Omega ,Cosmology: cosmological parameters ,(cosmology:) dark energy ,(cosmology:) cosmological parameters ,large-scale structure of Universe [Cosmology] ,galaxies ,0103 physical sciences ,cosmological parameters [Cosmology] ,Cosmology: large-scale structure of Universe ,observations [Cosmology] ,010303 astronomy & astrophysics ,milky-way ,Physics ,010308 nuclear & particles physics ,Oscillation ,Cosmology: dark energy ,Spectral density ,Astronomy and Astrophysics ,acoustic-oscillations ,redshift ,Redshift ,Baryon ,Space and Planetary Science ,cosmology: observations ,astro-ph.CO ,(cosmology:) large-scale structure of Universe ,dark energy [Cosmology] ,power-spectrum ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Zhao, Gong-Bo, et al., We perform a joint BAO and RSD analysis using the eBOSS DR16 LRG and ELG samples in the redshift range of z [0.6, 1.1], and detect an RSD signal from the cross-power spectrum at a ∼4σ confidence level, i.e., fσ8 = 0.317 ± 0.080 at zeff = 0.77. Based on the chained power spectrum, which is a new development in this work to mitigate the angular systematics, we measure the BAO distances and growth rate simultaneously at two effective redshifts, namely, DM/rd (z = 0.70) = 17.96 ± 0.51, DH/rd (z = 0.70) = 21.22 ± 1.20, fσ8 (z = 0.70) = 0.43 ± 0.05, and DM/rd (z = 0.845) = 18.90 ± 0.78, DH/rd (z = 0.845) = 20.91 ± 2.86, fσ8 (z = 0.845) = 0.30 ± 0.08. Combined with BAO measurements including those from the eBOSS DR16 QSO and Lyman-α sample, our measurement has raised the significance level of a non-zero ωΛ to ∼11σ. The data product of this work is publicly available at https://github.com/icosmology/eBOSS_DR16_LRGxELG and https://www.sdss.org/science/final-bao-and-rsd-measurements/., GBZ is supported by the National Key Basic Research and Development Program of China (No. 2018YFA0404503), and a grant of CAS Interdisciplinary Innovation Team. GBZ, YW, and WBZ are supported by NSFC Grants 11925303, 11720101004, 11673025, and 11890691. YW is also supported by the Nebula Talents Program of NAOC and by the Youth Innovation Promotion Association CAS. EMM has received funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (grant agreement no. 693024).
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36. Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G=18.5
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F. Anders, A. Khalatyan, A. B. A. Queiroz, C. Chiappini, J. Ardèvol, L. Casamiquela, F. Figueras, Ó. Jiménez-Arranz, C. Jordi, M. Monguió, M. Romero-Gómez, D. Altamirano, T. Antoja, R. Assaad, T. Cantat-Gaudin, A. Castro-Ginard, H. Enke, L. Girardi, G. Guiglion, S. Khan, X. Luri, A. Miglio, I. Minchev, P. Ramos, B. X. Santiago, M. Steinmetz, F. Anders, A. Khalatyan, A. B. A. Queiroz, C. Chiappini, J. Ardèvol, L. Casamiquela, F. Figueras, Ó. Jiménez-Arranz, C. Jordi, M. Monguió, M. Romero-Gómez, D. Altamirano, T. Antoja, R. Assaad, T. Cantat-Gaudin, A. Castro-Ginard, H. Enke, L. Girardi, G. Guiglion, S. Khan, X. Luri, A. Miglio, I. Minchev, P. Ramos, B. X. Santiago, M. Steinmetz, European Commission, and Ministerio de Ciencia e Innovación (España)
- Subjects
Stars: distance ,chemical-evolution ,Astrophysics - astrophysics of galaxies ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Galaxy - structure ,fundamental parameters [Stars] ,Astrophysics - solar and stellar astrophysics ,Stars - distances ,stellar content [Galaxy] ,Galaxy - general ,metal-poor stars ,Galaxy: general ,Galaxy: structure ,general [Galaxy] ,Astrophysics::Galaxy Astrophysics ,milky-way ,pristine survey ,Stars: fundamental parameters ,Solar and Stellar Astrophysics (astro-ph.SR) ,data release ,Galaxy: stellar content ,tagged groups ,Astronomy and Astrophysics ,distances [Stars] ,physical parameters ,machine-learning regression ,Space and Planetary Science ,giant branch ,Astrophysics of Galaxies (astro-ph.GA) ,stars: distances ,stellar metallicities ,Astrophysics::Earth and Planetary Astrophysics ,Galaxy - stellar content ,Stars - fundamental parameters ,structure [Galaxy] - Abstract
We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's early third data release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and AllWISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the {\tt StarHorse} code allow us to substantially improve the accuracy and precision over previous photo-astrometric stellar-parameter estimates. At magnitude $G=14\, (17)$, our typical precisions amount to 3% (15%) in distance, 0.13 mag (0.15 mag) in $V$-band extinction, and 140 K (180 K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface ({\tt gaia.aip.de}) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit make our results useful also beyond the next Gaia release, DR3., Comment: A&A, accepted, 27 pages, 25 figures. Fig. 5 has changed with respect to v1 (post-processing bug corrected). For various options to access the data see https://data.aip.de/projects/starhorse2021.html
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- 2021
- Full Text
- View/download PDF
37. Predicting far-infrared maps of galaxies via machine learning techniques
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Maarten Baes and Wouter Dobbels
- Subjects
FOS: Physical sciences ,Context (language use) ,Astrophysics ,SPECTRAL ENERGY-DISTRIBUTIONS ,Astrophysics::Cosmology and Extragalactic Astrophysics ,STAR-FORMATION RATES ,Machine learning ,computer.software_genre ,galaxies [infrared] ,Luminosity ,Far infrared ,RADIATIVE-TRANSFER ,Astrophysics::Solar and Stellar Astrophysics ,NEARBY GALAXIES ,Surface brightness ,Astrophysics::Galaxy Astrophysics ,Physics ,Luminous infrared galaxy ,HERSCHEL ,ISM [galaxies] ,business.industry ,ILLUSTRISTNG SIMULATIONS ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Wavelength ,DUST MASS ,Physics and Astronomy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,photometry [galaxies] ,Spectral energy distribution ,MILKY-WAY ,Artificial intelligence ,Astrophysics::Earth and Planetary Astrophysics ,business ,STELLAR MASS ,SKY SURVEY ,computer - Abstract
The ultraviolet (UV) to sub-millimetre (submm) spectral energy distribution of galaxies can be roughly divided into two sections: the stellar emission (attenuated by dust) at UV to near-infrared wavelengths and dust emission at longer wavelengths. In Dobbels et al. (2020), we show that these two sections are strongly related, and we can predict the global dust properties from the integrated UV to mid-infrared emission with the help of machine learning techniques. We investigate if these machine learning techniques can also be extended to resolved scales. Our aim is to predict resolved maps of the specific dust luminosity, specific dust mass, and dust temperature starting from a set of surface brightness images from UV to mid-infrared wavelengths. We used a selection of nearby galaxies retrieved from the DustPedia sample, in addition to M31 and M33. These were convolved and resampled to a range of pixel sizes, ranging from 150 pc to 3 kpc. We trained a random forest model which considers each pixel individually. We find that the predictions work well on resolved scales, with the dust mass and temperature having a similar root mean square error as on global scales (0.32 dex and 3.15 K on 18" scales respectively), and the dust luminosity being noticeably better (0.11 dex). We find no significant dependence on the pixel scale. Predictions on individual galaxies can be biased, and we find that about two-thirds of the scatter can be attributed to scatter between galaxies (rather than within galaxies). A machine learning approach can be used to create dust maps, with its resolution being only limited to the input bands, thus achieving a higher resolution than Herschel. These dust maps can be used to improve global estimates of dust properties, they can lead to a better estimate of dust attenuation, and they can be used as a constraint on cosmological simulations that trace dust., Comment: 16 pages, 13 figures, accepted by A&A
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- 2021
- Full Text
- View/download PDF
38. The volumetric star formation law for nearby galaxies
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Filippo Fraternali, Gabriele Pezzulli, Antonino Marasco, Cecilia Bacchini, and Astronomy
- Subjects
Work (thermodynamics) ,galaxies: spiral ,SCHMIDT-LAW ,Milky Way ,ISM: structure ,ULTRAVIOLET ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Disc galaxy ,01 natural sciences ,FORMATION THRESHOLDS ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Dwarf galaxy ,Physics ,Spiral galaxy ,stars: formation ,010308 nuclear & particles physics ,Star formation ,Astronomy and Astrophysics ,galaxies: dwarf ,Astrophysics - Astrophysics of Galaxies ,GAS ACCRETION ,Galaxy ,formation ,galaxies: star formation ,galaxies: structure [stars] ,FORMATION RATES ,MOLECULAR GAS ,Volume (thermodynamics) ,Space and Planetary Science ,EDGE ,Astrophysics of Galaxies (astro-ph.GA) ,Law ,ROTATION CURVES ,galaxies: structure ,MILKY-WAY ,SHAPE - Abstract
In the last decades, much effort has been put into finding the star formation law which could unequivocally link the gas and the star formation rate (SFR) densities measured on sub-kiloparsec scale in star-forming galaxies. The conventional approach of using the observed surface densities to infer star formation laws has however revealed a major and well-known issue, as such relations are valid for the high-density regions of galaxies but break down in low-density and HI-dominated environments. Recently, an empirical correlation between the total gas (HI+H$_2$) and the star formation rate (SFR) volume densities was obtained for a sample of nearby disc galaxies and for the Milky Way. This volumetric star formation (VSF) law is a single power-law with no break and a smaller intrinsic scatter with respect to the star formation laws based on the surface density. In this work, we explore the VSF law in the regime of dwarf galaxies in order to test its validity in HI-dominated, low-density, and low-metallicity environments. In addition, we assess this relation in the outskirts of spiral galaxies, which are low-density and HI-dominated regions similar to dwarf galaxies. Remarkably, we find the VSF law, namely $\rho_\mathrm{SFR} \propto \rho_\mathrm{gas}^\alpha$ with $\alpha \approx 2$, is valid for both these regimes. This result indicates that the VSF law, which holds unbroken for a wide range of gas ($\approx 3$ dex) and SFR ($\approx 6$ dex) volume densities, is the empirical relation with the smallest intrinsic scatter and is likely more fundamental than surface-based star formation laws., Comment: 17 pages, 7 figures, accepted by A&A
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- 2020
39. Weighing the Galactic disk in sub-regions of the solar neighbourhood using Gaia DR2
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Giacomo Monari, Axel Widmark, P. F. de Salas, Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
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SDSS ,MODELS ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Galaxy: disk ,DARK-MATTER DENSITY ,0103 physical sciences ,Disc ,010303 astronomy & astrophysics ,Neighbourhood (mathematics) ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,solar neighborhood ,LOCAL-DENSITY ,Astronomy and Astrophysics ,Astrometry ,kinematics and dynamics [Galaxy] ,Sub region ,Astrophysics - Astrophysics of Galaxies ,GALAXY ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,SURFACE MASS DENSITY ,MILKY-WAY ,astrometry ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,disk [Galaxy] ,Galaxy: kinematics and dynamics ,STARS - Abstract
We infer the gravitational potential of the Galactic disk by analysing the phase-space densities of 120 stellar samples in 40 spatially separate sub-regions of the solar neighbourhood, using Gaia's second data release (DR2), in order to quantify spatially dependent systematic effects that bias this type of measurement. The gravitational potential was inferred under the assumption of a steady state in the framework of a Bayesian hierarchical model. We performed a joint fit of our stellar tracers' three-dimensional velocity distribution, while fully accounting for the astrometric uncertainties of all stars. The inferred gravitational potential is compared, post-inference, to a model for the baryonic matter and halo dark matter components. We see an unexpected but clear trend for all 40 spatially separate sub-regions: Compared to the potential derived from the baryonic model, the inferred gravitational potential is significantly steeper close to the Galactic mid-plane (, 19 pages, 17 figures, accepted for publication in A&A
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- 2020
40. CHIMPS2: Survey description and $^{12}$CO emission in the Galactic Centre
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Hongsu Kim, Yong-Hyun Lee, H. Shi, Hsin-Yi Chen, Sarah Ragan, Gary A. Fuller, Xindi Tang, Francisca Kemper, H. S. Thomas, Sarah Graves, A. Y. Yang, Tetsuhiro Minamidani, Hyeong Sik Yun, Eric W. Koch, David Eden, Jungyeon Cho, Per Friberg, Manash R. Samal, I. Han, S. N. Longmore, Paul C. Clark, T. C. Ching, K. Tahani, Z. Chen, Erik Rosolowsky, M. Zhu, Chengcui Zhang, Sanjay Srinivasan, Kee-Tae Kim, D. L. Li, Jae-Woo Kim, J. Yuan, Masato I. N. Kobayashi, N. T. Phuong, R. Rani, X. J. Jiang, N. Yue, M. Zhang, C. H. Yan, Soumen Deb, Christopher M. Brunt, S. Mairs, M. Liu, A. Bemis, Alessio Traficante, Chang-Sheng Shi, L. W. Liao, Ana Duarte-Cabral, A. Trejo, Andrew Rigby, G. Violino, Shih-Ping Lai, L. Qian, L. Yuan, Nicolas Peretto, Sheng-Yuan Liu, Y. Su, Tie Liu, Tomofumi Umemoto, Kazufumi Torii, Jeong-Eun Lee, S. Wallström, Claudia Cyganowski, Z. Pan, P. Tuan-Anh, Y. Sun, Nario Kuno, Gilles Joncas, Peter Scicluna, Geumsook Park, Takuya Fujiyoshi, M. J. Currie, B. Wang, Y. Gao, Mark Thompson, S. Zhang, K. M. Lacialle, C. H. Peñaloza, Rene Plume, Jaime E. Pineda, Yi-Jehng Kuan, Y. F. Wu, J. Campbell-White, James Urquhart, Toby J. T. Moore, J. J. Zhou, E. Puspitaningrum, Jonathan D. Henshaw, Ho-Gyu Lee, Chang Won Lee, N. Izumi, Y. Ao, Woojin Kwon, S. L. Kim, H. Ma, Eun Jung Chung, Archana Soam, Q. H. Tan, C. Figura, Glenn J. White, S. J. Billington, O. Morata, C. Zhou, Melvin Hoare, Harriet Parsons, M. Fich, and University of St Andrews. School of Physics and Astronomy
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molecular data ,SPIRAL ARMS ,FOS: Physical sciences ,PHYSICAL-PROPERTIES ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,I ,01 natural sciences ,CENTRAL MOLECULAR ZONE ,STAR-FORMATION ,surveys ,0103 physical sciences ,QB Astronomy ,QD ,010303 astronomy & astrophysics ,RADIO-CONTINUUM ,QC ,Solar and Stellar Astrophysics (astro-ph.SR) ,molecules [ISM] ,Astrophysics::Galaxy Astrophysics ,QB ,Physics ,HI-GAL ,Science & Technology ,formation [stars] ,010308 nuclear & particles physics ,CLOUDS ,Astronomy ,Astronomy and Astrophysics ,3rd-DAS ,QD Chemistry ,SAGITTARIUS-D ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,centre [Galaxy] ,Stars ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Physical Sciences ,MILKY-WAY - Abstract
The latest generation of Galactic-plane surveys is enhancing our ability to study the effects of galactic environment upon the process of star formation. We present the first data from CO Heterodyne Inner Milky Way Plane Survey 2 (CHIMPS2). CHIMPS2 is a survey that will observe the Inner Galaxy, the Central Molecular Zone (CMZ), and a section of the Outer Galaxy in $^{12}$CO, $^{13}$CO, and C$^{18}$O $(J = 3\rightarrow2)$ emission with the Heterodyne Array Receiver Program on the James Clerk Maxwell Telescope (JCMT). The first CHIMPS2 data presented here are a first look towards the CMZ in $^{12}$CO J = 3$\rightarrow$2 and cover $-3^{\circ}\leq\,\ell\,\leq\,5^{\circ}$ and $\mid$b$\mid \leq 0.5^{\circ}$ with angular resolution of 15 arcsec, velocity resolution of 1 km s$^{-1}$, and rms $\Delta T_A ^\ast =$ 0.58 K at these resolutions. Such high-resolution observations of the CMZ will be a valuable data set for future studies, whilst complementing the existing Galactic Plane surveys, such as SEDIGISM, the Herschel infrared Galactic Plane Survey, and ATLASGAL. In this paper, we discuss the survey plan, the current observations and data, as well as presenting position-position maps of the region. The position-velocity maps detect foreground spiral arms in both absorption and emission., Comment: 18 pages, 14 figures, accepted for publication in MNRAS
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- 2020
41. Implications for dark matter direct detection in the presence of LIGO-motivated primordial black holes
- Author
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Mark P. Hertzberg, Enrico D. Schiappacasse, Tsutomu T. Yanagida, and Helsinki Institute of Physics
- Subjects
High Energy Physics - Theory ,DISRUPTION ,HALO MODELS ,Primordial black hole ,Astrophysics ,Dark mini-halos ,dark matter direct detection ,kosmologia ,01 natural sciences ,General Relativity and Quantum Cosmology ,LIMITS ,High Energy Physics - Phenomenology (hep-ph) ,Bulge ,Physics ,primordial black holes ,lcsh:QC1-999 ,High Energy Physics - Phenomenology ,BULGE ,MILKY-WAY ,LIGO-Virgo collaboration ,Halo ,Astrophysics - Cosmology and Nongalactic Astrophysics ,axion dark matter ,Nuclear and High Energy Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Axion dark matter ,Milky Way ,Dark matter ,mustat aukot ,FOS: Physical sciences ,Primordial black holes ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Dark matter direct detection ,114 Physical sciences ,pimeä aine ,dark mini-halos ,0103 physical sciences ,010306 general physics ,Axion ,CP CONSERVATION ,Astrophysics::Galaxy Astrophysics ,010308 nuclear & particles physics ,CONSTRAINTS ,Astrophysics - Astrophysics of Galaxies ,LIGO ,Galaxy ,High Energy Physics - Theory (hep-th) ,Astrophysics of Galaxies (astro-ph.GA) ,lcsh:Physics - Abstract
We discuss formation of dark matter (DM) mini-halos around primordial black holes (PBHs) and its implication on DM direct detection experiments, including axion searches. Motivated by LIGO observations, we consider $f_{\textrm{DM}} \simeq 0.01$ as the fraction of DM in PBHs with masses $10 M_{\odot} - 70 M_{\odot}$. In this case, we expect the presence of dressed PBHs after Milky Way halo formation with mini-halo masses peaked around $M_{\textrm{halo}} \sim (50-55) M_{\textrm{PBH}}$. We analyze the effect of tidal forces acting on dressed PBHs within the Milky Way galaxy. In the solar neighborhood, the mini-halos are resistant against tidal disruption from the mean-field potential of the galaxy and encounters with stars, but they undergo a small level of disruption caused by disk shocking. The presence of mini-halos around LIGO-motivated PBHs today could reduce by half the local dark matter background. High-resolution simulations are encouraged. If the proposed scenario is realized, chances of direct detection of DM would decrease., Comment: 9 pages, 3 figures. v2: New material added, especially in Secs. 2.2-2.3. References added. v3: Updated towards version accepted in Physics Letters B
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- 2020
42. ATOMS : ALMA three-millimeter observations of massive star-forming regions - II. Compact objects in ACA observations and star formation scaling relations
- Author
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Paul F. Goldsmith, Feng-Yao Zhu, Sheng-Yuan Liu, Di Li, Feng-Wei Xu, Pak Shing Li, Jingwen Wu, Mika Juvela, Maria Cunningham, Qiu-Yi Luo, Zhiyuan Ren, Sheng-Li Qin, Qizhou Zhang, Sung-ju Kang, Hyeong-Sik Yun, X.-W. Liu, Yu Wang, Chao Zhang, Diego Mardones, Shanghuo Li, Neal J. Evans, Ken'ichi Tatematsu, Ya-Ping Peng, L. Viktor Tóth, Yuefang Wu, Isabelle Ristorcelli, Hee-Weon Yi, Kee-Tae Kim, Tie Liu, Ke Wang, Jeong-Eun Lee, Anandmayee Tej, Guido Garay, Tomoya Hirota, Chang Won Lee, Leonardo Bronfman, Zhi-Qiang Shen, Junzhi Wang, Namitha Issac, Juan Li, Yong Zhang, Hong-Li Liu, T. Baug, Department of Physics, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Shanghai Astronomical Observatory [Shanghai] (SHAO), and Chinese Academy of Sciences [Beijing] (CAS)
- Subjects
TRACERS ,Milky Way ,FOS: Physical sciences ,Star (graph theory) ,01 natural sciences ,ISM: clouds ,CLUMPS ,clouds -ISM ,DENSE MOLECULAR GAS ,Observatory ,galaxies ,0103 physical sciences ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,formation -ISM ,Physics ,stars: formation ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,Star formation ,formation ,Astronomy ,Astronomy and Astrophysics ,115 Astronomy, Space science ,Chinese academy of sciences ,Astrophysics - Astrophysics of Galaxies ,ISM: molecules ,HCN ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,galaxies: star formation ,MILKY-WAY ,Christian ministry ,Millimeter ,[SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] ,molecules -stars - Abstract
We report studies of the relationships between the total bolometric luminosity ($L_{\rm bol}$ or $L_{\rm TIR}$) and the molecular line luminosities of $J=1-0$ transitions of H$^{13}$CN, H$^{13}$CO$^+$, HCN, and HCO$^+$ with data obtained from ACA observations in the "ATOMS" survey of 146 active Galactic star forming regions. The correlations between $L_{\rm bol}$ and molecular line luminosities $L'_{\rm mol}$ of the four transitions all appear to be approximately linear. Line emission of isotopologues shows as large scatters in $L_{\rm bol}$-$L'_{\rm mol}$ relations as their main line emission. The log($L_{\rm bol}$/$L'_{\rm mol}$) for different molecular line tracers have similar distributions. The $L_{\rm bol}$-to-$L'_{\rm mol}$ ratios do not change with galactocentric distances ($R_{\rm GC}$) and clump masses ($M_{\rm clump}$). The molecular line luminosity ratios (HCN-to-HCO$^+$, H$^{13}$CN-to-H$^{13}$CO$^+$, HCN-to-H$^{13}$CN and HCO$^+$-to-H$^{13}$CO$^+$) all appear constant against $L_{\rm bol}$, dust temperature ($T_{\rm d}$), $M_{\rm clump}$ and $R_{\rm GC}$. Our studies suggest that both the main lines and isotopologue lines are good tracers of the total masses of dense gas in Galactic molecular clumps. The large optical depths of main lines do not affect the interpretation of the slopes in star formation relations. We find that the mean star formation efficiency (SFE) of massive Galactic clumps in the "ATOMS" survey is reasonably consistent with other measures of the SFE for dense gas, even those using very different tracers or examining very different spatial scales., Comment: Published on MNRAS. The full tables are included in Tables.pdf or Tables.tex files, which can be downloaded from source files
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- 2020
43. 'Observations' of simulated dwarf galaxies: Star-formation histories from color-magnitude diagrams
- Author
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Carme Gallart, Michele Mastropietro, Robbert Verbeke, Shivangee Rathi, Edouard J. Bernard, Sven De Rijcke, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,dwarf [galaxies] ,Milky Way ,MODELS ,Extinction (astronomy) ,Hertzsprung–Russell and C–M diagrams ,CODE ,FOS: Physical sciences ,POPULATION SYNTHESIS ,DUST ,Context (language use) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,I ,01 natural sciences ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,evolution [galaxies] ,Astrophysics::Galaxy Astrophysics ,Dwarf galaxy ,Physics ,010308 nuclear & particles physics ,Star formation ,James Webb Space Telescope ,Astronomy and Astrophysics ,galaxies: dwarf ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Physics and Astronomy ,Space and Planetary Science ,galaxies: star formation ,Astrophysics of Galaxies (astro-ph.GA) ,Magnitude (astronomy) ,Hertzsprung-Russell and C-M diagrams ,MILKY-WAY ,Astrophysics::Earth and Planetary Astrophysics ,star formation [galaxies] ,STELLAR EVOLUTION DATABASE ,galaxies: evolution ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Apparent deviations between properties of dwarf galaxies from observations and simulations are known to exist, such as the "Missing Dwarfs" problem, the too-big-to-fail problem, and the cusp-core problem, to name a few. Recent studies have shown that these issues can at least be partially resolved by taking into account the systematic differences between simulations and observations. This work aims to investigate and address any systematic differences affecting the comparison of simulations with observations. To this aim, we analyzed a set of 24 realistically simulated MoRIA (Models of Realistic dwarfs In Action) dwarf galaxies in an observationally motivated way. We first constructed "observed" color-magnitude diagrams (CMDs) of the simulated dwarf galaxies in the typically used V- and I-bands. Then we used the CMD-fitting method to recover their star-formation histories (SFHs) from their observed CMDs. These solved SFHs were then directly compared to the true SFHs from the simulation star-particle data, mainly in terms of the star-formation rate(SFR) and the age-metallicity relation (AMR). We applied a dust extinction prescription to the simulation data to produce observed CMDs affected by dust in star-formation regions. Since future facilities, such as the JWST and E-ELT will focus on the near IR rather than the optical, we also constructed and analyzed CMDs using the I- and H-bands. We find a very good agreement between the recovered and the true SFHs of all the simulated dwarf galaxies in our sample, from the synthetic CMD analysis of their V-I versus I as well as the I-H versus H CMDs. Dust leads to an underestimation of the SFR during the last few hundred million years. Overall, our analysis indicates that quantities like SFR and AMR derived from the photometric observations of galaxies are directly comparable to their simulated counterparts., 19 pages, 15 figures, to appear in Section 4. Extragalactic astronomy of Astronomy and Astrophysics
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- 2020
44. An all-sky proper-motion map of the Sagittarius stream using Gaia DR2
- Author
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Cecilia Mateu, Friedrich Anders, Julio A. Carballo-Bello, Carme Jordi, P. Ramos, Amina Helmi, Teresa Antoja, Astronomy, European Commission, Ministerio de Economía y Competitividad (España), Universidad de Barcelona, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Agencia Estatal de Investigación (España), and Ministerio de Ciencia, Innovación y Universidades (España)
- Subjects
Galaxy: haloGalaxy: kinematics and dynamics ,Proper motion ,Milky Way ,media_common.quotation_subject ,Population ,FOS: Physical sciences ,Astrophysics ,Sagittarius Stream ,Astrophysics::Cosmology and Extragalactic Astrophysics ,MASS ,01 natural sciences ,VIEW ,0103 physical sciences ,education ,010303 astronomy & astrophysics ,Red clump ,Astrophysics::Galaxy Astrophysics ,SATELLITE ,media_common ,Physics ,education.field_of_study ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Astrometry ,galaxies: dwarf ,Astrophysics - Astrophysics of Galaxies ,CATALOG ,haloGalaxy: kinematics and dynamics [Galaxy] ,CLOUD ,Galaxy: halo ,dwarf [Galaxies] ,Stars ,DWARF GALAXY ,formation [Galaxy] ,Space and Planetary Science ,Sky ,Galaxy: formation ,Astrophysics of Galaxies (astro-ph.GA) ,DISCOVERY ,astrometry ,MILKY-WAY ,Galaxy: kinematics and dynamics ,GALACTIC HALO ,STARS - Abstract
[Aims]: We aim to measure the proper motion along the Sagittarius stream, which is the missing piece in determining its full 6D phase space coordinates. [Methods]: We conduct a blind search of over-densities in proper motion from the Gaia second data release in a broad region around the Sagittarius stream by applying wavelet transform techniques. [Results]: We find that for most of the sky patches, the highest intensity peaks delineate the path of the Sagittarius stream. The 1500 peaks identified depict a continuous sequence spanning almost 2π in the sky, only obscured when the stream crosses the Galactic disk. Altogether, around 100 000 stars potentially belong to the stream as indicated by a coarse inspection of the color-magnitude diagrams. From these stars, we determine the proper motion along the Sagittarius stream, making it the proper-motion sequence with the largest span and continuity ever measured for a stream. A first comparison with existing N-body models of the stream reveals some discrepancies, especially near the pericenter of the trailing arm and an underestimation of the total proper motion for the leading arm. [Conclusions]: Our study provides a starting point for determining the variation of the population of stars along the stream, the distance to the stream from the red clump stars, and the solar motion. It also permits much more accurate measurement of the Milky Way potential., This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos. esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 745617 and No. 800502. This work was supported by the MINECO (Spanish Ministry of Economy) through grant ESP2016-80079-C2-1-R and RTI2018-095076-B-C21 (MINECO/FEDER, UE), and MDM-2014-0369 of ICCUB (Unidad de Excelencia “María de Maeztu”). This project has received support from the DGAPA/UNAM PAPIIT program grant IG100319. AH acknowledges financial support from a VICI grant from the Netherlands Organisation for Scientific Research, NWO. JAC-B acknowledges financial support to CAS-CONICYT 17003.
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- 2020
45. Dynamical Equilibrium in the Molecular ISM in 28 Nearby Star-Forming Galaxies
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Daniel A. Dale, Kathryn Grasha, Sharon Meidt, Jiayi Sun, Eve C. Ostriker, Alberto D. Bolatto, I-Da Chiang, Karin Sandstrom, Janice C. Lee, Eric Emsellem, Toshiki Saito, Jonathan D. Henshaw, Dyas Utomo, Cinthya N. Herrera, Antonio Usero, Erik Rosolowsky, Simon C. O. Glover, Frank Bigiel, Jérôme Pety, Annie Hughes, Andreas Schruba, María J. Jiménez-Donaire, Christopher Faesi, Miguel Querejeta, Guillermo A. Blanc, Mélanie Chevance, J. M. Diederik Kruijssen, Adam K. Leroy, Eva Schinnerer, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
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010504 meteorology & atmospheric sciences ,Interstellar dynamics ,Funding grant ,FOS: Physical sciences ,Library science ,Astrophysics::Cosmology and Extragalactic Astrophysics ,PRESSURE ,MASS ,01 natural sciences ,MAGNETIC-FIELDS ,Atomic energy commission ,German ,3-DIMENSIONAL DISTRIBUTION ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,INTERSTELLAR-MEDIUM ,European research ,Star formation ,CLOUDS ,GAS CONTENT ,Astronomy and Astrophysics ,Interstellar molecules ,Astrophysics - Astrophysics of Galaxies ,language.human_language ,Physics and Astronomy ,[SDU]Sciences of the Universe [physics] ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,SUPERNOVA FEEDBACK ,language ,MILKY-WAY ,TURBULENCE - Abstract
We compare the observed turbulent pressure in molecular gas, $P_\mathrm{turb}$, to the required pressure for the interstellar gas to stay in equilibrium in the gravitational potential of a galaxy, $P_\mathrm{DE}$. To do this, we combine arcsecond resolution CO data from PHANGS-ALMA with multi-wavelength data that traces the atomic gas, stellar structure, and star formation rate (SFR) for 28 nearby star-forming galaxies. We find that $P_\mathrm{turb}$ correlates with, but almost always exceeds the estimated $P_\mathrm{DE}$ on kiloparsec scales. This indicates that the molecular gas is over-pressurized relative to the large-scale environment. We show that this over-pressurization can be explained by the clumpy nature of molecular gas; a revised estimate of $P_\mathrm{DE}$ on cloud scales, which accounts for molecular gas self-gravity, external gravity, and ambient pressure, agrees well with the observed $P_\mathrm{turb}$ in galaxy disks. We also find that molecular gas with cloud-scale ${P_\mathrm{turb}}\approx{P_\mathrm{DE}}\gtrsim{10^5\,k_\mathrm{B}\,\mathrm{K\,cm^{-3}}}$ in our sample is more likely to be self-gravitating, whereas gas at lower pressure appears more influenced by ambient pressure and/or external gravity. Furthermore, we show that the ratio between $P_\mathrm{turb}$ and the observed SFR surface density, $\Sigma_\mathrm{SFR}$, is compatible with stellar feedback-driven momentum injection in most cases, while a subset of the regions may show evidence of turbulence driven by additional sources. The correlation between $\Sigma_\mathrm{SFR}$ and kpc-scale $P_\mathrm{DE}$ in galaxy disks is consistent with the expectation from self-regulated star formation models. Finally, we confirm the empirical correlation between molecular-to-atomic gas ratio and kpc-scale $P_\mathrm{DE}$ reported in previous works., Comment: 28 pages + 3 appendices, ApJ in press. See https://www.youtube.com/watch?v=qxkd-RXB0Ek for a short video describing the main results. Data tables available at https://www.canfar.net/storage/list/phangs/RELEASES/Sun_etal_2020 prior to publication
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- 2020
46. The headlight cloud in NGC 628 : an extreme giant molecular cloud in a typical galaxy disk
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Alexander P. S. Hygate, Cinthya N. Herrera, Dyas Utomo, Mélanie Chevance, Kathryn Kreckel, Antonio Usero, Jiayi Sun, Ismael Pessa, Daniel A. Dale, Simon C. O. Glover, Andreas Schruba, Sharon E. Meidt, Jérôme Pety, Kathryn Grasha, Diane Cormier, Adam K. Leroy, Toshiki Saito, Frank Bigiel, Annie Hughes, Miguel Querejeta, Eva Schinnerer, Philipp Lang, Guillermo A. Blanc, Erik Rosolowsky, J. M. Diederik Kruijssen, Christopher Faesi, María J. Jiménez-Donaire, Kazimierz Sliwa, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), European Southern Observatory (ESO), Observatorio Astronomico Nacional, Madrid, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Carnegie Observatories, Carnegie Institution for Science, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg] = Heidelberg University, University of Wyoming (UW), Australian National University (ANU), Ohio State University [Columbus] (OSU), University of Alberta, Max-Planck-Institut für Extraterrestrische Physik (MPE), Programme National 'Physique et Chimie du Milieu Interstellaire' (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES., Programme National Cosmology and Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES., European Union’s Horizon 2020 research and innovation programme (grant agreement No726384)., European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907)., Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent, Harvard University [Cambridge]-Smithsonian Institution, Carnegie Institution for Science [Washington], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universidad de Chile, Universität Heidelberg [Heidelberg], PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and The Observatories of the Carnegie Institution for Science
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HII regions ,Stellar population ,FOS: Physical sciences ,Context (language use) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,I ,ISM: clouds ,01 natural sciences ,Galaxy: disk ,STAR-FORMATION ,0103 physical sciences ,NEARBY GALAXIES ,Disc ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,SPIRAL STRUCTURE ,stars: formation ,Spiral galaxy ,formation [stars] ,010308 nuclear & particles physics ,Star formation ,Molecular cloud ,Astronomy and Astrophysics ,kinematics and dynamics [Galaxy] ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,CO ,Stars ,STELLAR CLUSTERS ,Physics and Astronomy ,13. Climate action ,Space and Planetary Science ,GAS ,Astrophysics of Galaxies (astro-ph.GA) ,MILKY-WAY ,PATTERN SPEEDS ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Galaxy: kinematics and dynamics ,clouds [ISM] ,disk [Galaxy] ,UNCERTAINTY PRINCIPLE - Abstract
Cloud-scale surveys of molecular gas reveal the link between molecular clouds properties and star formation (SF) across a range of galactic environments. Cloud populations in galaxy disks are considered to be representative of the `normal' SF. At high resolution, however, clouds with exceptional gas properties and SF activity may also be observed in normal disk environments. In this paper, we study the brightest cloud traced in CO emission in the disk of NGC628. The cloud is spatially coincident with an extremely bright HII region. We characterize its molecular gas properties and investigate how feedback and large-scale processes influence the properties of the molecular gas. High resolution CO ALMA observations are used to characterize its mass and dynamical state, which are compared to other clouds in NGC628. A LVG analysis is used to constrain the beam-diluted density and temperature of the molecular gas. We analyze the MUSE spectrum using Starburst99 to characterize the young stellar population associated with the HII region. The cloud is massive ($1-2\times10^7$M$_{\odot}$), with a beam-diluted density of $n_{\rm H_2}=5\times10^4$ cm$^{-3}$. It has a low virial parameter, suggesting that its CO emission may be overluminous due to heating by the HII region. A young ($2-4$ Myr), massive $3\times10^{5}$ M$_{\odot}$ stellar population is associated. We argue that the cloud is currently being destroyed by feedback from young massive stars. Due to the cloud's large mass, this phase of the cloud's evolution is long enough for the impact of feedback on the excitation of the gas to be observed. Its high mass may be related to its location at a spiral co-rotation radius, where gas experiences reduced galactic shear compared to other regions of the disk, and receives a sustained inflow of gas that can promote the cloud's mass growth., Comment: A&A accepted
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- 2020
47. Gaia Early Data Release 3: Acceleration of the solar system from Gaia astrometry
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Vincenzo Ripepi, P. Gavras, M. Vaillant, Mathias Schultheis, László Molnár, E. Poujoulet, Mark Cropper, C. Babusiaux, D. Molina, J. Fernández-Hernández, G. Jevardat de Fombelle, A. de Torres, Aldo Dell'Oro, J. Castañeda, Z. Kostrzewa-Rutkowska, A. Bombrun, André Moitinho, Marcella Marconi, Rossella Cancelliere, M. Hauser, M. Ajaj, C. M. Raiteri, L. Eyer, Michał Pawlak, H. I. Siddiqui, C. Ducourant, Tatiana Muraveva, Tsevi Mazeh, A. Panahi, Federico Marocco, Stefano Bertone, D. Vicente, Patrick Charlot, A. Guerrier, R. De March, Mario Gai, J. Souchay, H. E. P. Lindstrøm, Nicoletta Sanna, Agnes Fienga, Giovanni Comoretto, Jon Marchant, A. Lorca, E. Utrilla, A. Garcia-Gutierrez, Ilaria Musella, L. Balaguer-Núñez, Leanne P. Guy, N. Leclerc, E. Brugaletta, A. Yoldas, Harry Enke, Rosanna Sordo, Zoltan Balog, H. E. Huckle, L. Palaversa, Monica Rainer, T. A. Lister, F. A. Jansen, Ruth Carballo, Alessandro Spagna, J. M. Carrasco, Mikael Granvik, Derek W. Morris, F. Julbe, A. Hutton, J. Osinde, D. W. Evans, M. van Leeuwen, M. Weiler, F. Thévenin, F. Torra, Iain A. Steele, Lorenzo Rimoldini, Alessandro Sozzetti, Francesca Fragkoudi, K. Janßen, O. L. Creevey, J. González-Núñez, T. Pauwels, R. Buzzi, Miguel García-Torres, S. Liao, G. Tauran, Lennart Lindegren, C. Fouron, Pierre Fernique, Céline Reylé, P. Di Matteo, E. Szegedi-Elek, F. Pailler, Stefan Jordan, Roberto Molinaro, Elisabetta Caffau, Federica Spoto, Felix Franke, D. Barbato, Isabelle Lecoeur-Taïbi, Tristan Cantat-Gaudin, Alejandra Recio-Blanco, E. Livanou, W. Roux, X. Peñalosa Esteller, P. A. Palicio, J. H. J. de Bruijne, Sergi Blanco-Cuaresma, Deborah Busonero, F. Riclet, Conny Aerts, Georges Kordopatis, Guy Rixon, F. Solitro, Davide Massari, Mike Smith, D. Baines, Roberto Morbidelli, Gerry Gilmore, G. Plum, Alexey Mints, O. Marchal, Juan Zorec, Ángel Gómez, C. A. Stephenson, Michael Davidson, C. Fabricius, E. Licata, Sergio Messina, Laszlo Szabados, M. Biermann, A. Garofalo, G. Holland, F. De Angeli, Andreas Korn, E. Anglada Varela, Grigori Fedorets, S. Girona, E. Gerlach, Antonella Vallenari, M. Riello, Łukasz Wyrzykowski, Damien Ségransan, F. Taris, L. Bramante, Alberto Cellino, S. Regibo, Andrej Prsa, M. Sarasso, E. Poggio, W. Löffler, Paolo Giacobbe, Jordi Portell, Elisa Distefano, Eric Slezak, I. Bellas-Velidis, Nicolas Rambaux, E. Balbinot, J.-B. Delisle, Maroussia Roelens, E. Salguero, P. de Teodoro, E. van Dillen, Y. Lebreton, Francois Mignard, Sergei A. Klioner, Ulrich Bastian, N. Samaras, G. Orrù, R. E. de Souza, P. Esquej, Paul J. McMillan, A. C. Lanzafame, Sébastien Lambert, Beatrice Bucciarelli, Jose M Hernandez, M. Bernet, S. Ragaini, Gisella Clementini, A. F. Mulone, Ludovic Delchambre, C. Panem, Eric Gosset, P. David, M. Garcia-Reinaldos, Ana Ulla, F. Crifo, J. Guiraud, Mariateresa Crosta, L. Chaoul, C. Diener, Carlos Dafonte, Karri Muinonen, Alex Lobel, J.-L. Bassilana, Maria Süveges, Isabella Pagano, Dimitri Pourbaix, D. Eappachen, M. Haywood, R. Drimmel, Y. Viala, S. Voutsinas, D. Semeux, William Thuillot, N. A. Walton, Paolo Montegriffo, A. Abreu Aramburu, C. Fabre, H. Zhao, Alessandro Bressan, S. Bouquillon, Sanjeev Khanna, T. Lebzelter, N. Tonello, L. Siltala, M. G. Lattanzi, C. Crowley, P. Yvard, Carme Jordi, Elena Pancino, E. del Pozo, Jan Rybizki, Nami Mowlavi, C. Barache, Morgan Fouesneau, J. De Ridder, Ugo Becciani, Martin Altmann, F. van Leeuwen, P. M. Marrese, M. A. Álvarez, A. Jean-Antoine Piccolo, A. F. Lanza, Alberto Vecchiato, Thomas Wevers, Caroline Soubiran, C. P. Murphy, A. M. Piersimoni, Alessandra Mastrobuono-Battisti, Peter G. Jonker, A. Sagristà Sellés, T. Roegiers, S. Marinoni, Johannes Sahlmann, Rene Andrae, P. Sartoretti, G. Altavilla, Raphael Guerra, F. X. Pineau, M. Segol, T. Prusti, J. J. González-Vidal, J. J. Aguado, N. R. Millar, A. Baudesson-Stella, Andrea Chiavassa, Laurent Chemin, C. Turon, H. Steidelmüller, Douglas J. Marshall, A. G. Butkevich, Alberto Riva, P. de Laverny, Simchon Faigler, Laurent Galluccio, A. Mora, P. Re Fiorentin, C. Ordénovic, J. F. Le Campion, A. Delgado, V. Sanchez Gimenez, M. David, G. Sadowski, R. L. Smart, A. Masip, Laia Casamiquela, R. Messineo, R. Mor, J. Bakker, C. Dolding, J. M. Martín-Fleitas, S. Diakite, Coryn A. L. Bailer-Jones, D. Souami, P. Madrero Pardo, Martin A. Barstow, David Teyssier, Ummi Abbas, Jesus Salgado, Paolo Tanga, A. Burlacu, O. Vanel, Ulrike Heiter, Daniel Hestroffer, Sebastian L. Hidalgo, H. E. Delgado, Alberto Krone-Martins, C. Robin, Kevin Benson, Christos Siopis, S. Managau, P. Burgess, Tomaz Zwitter, M. M. S. Marcos Santos, S. Cowell, J. L. Halbwachs, Xavier Luri, Antti Penttilä, R. Geyer, Minia Manteiga, Yassine Damerdji, Nigel Hambly, S. Bartolomé, J. Álvarez Cid-Fuentes, P. Osborne, J. Juaristi Campillo, Mark Taylor, Richard I. Anderson, Y. Le Fustec, Thierry Morel, T. Cornez, Krzysztof A. Rybicki, L. Pulone, N. Bauchet, Pierre Kervella, C. Zurbach, Alfred Castro-Ginard, Frédéric Arenou, P. Ramos, Robert G. Mann, Annie C. Robin, J. C. Segovia, M. Barros, Hector Canovas, D. L. Harrison, Y. Lasne, L. Noval, David Hobbs, E. F. del Peloso, P. Castro Sampol, Yves Fremat, F. De Luise, Daniel Michalik, P. J. Richards, L. Karbevska, N. Hładczuk, K. Kruszyńska, T. Boch, Sofia Randich, A. G. A. Brown, C. Pagani, L. Martin Polo, M. Ramos-Lerate, Krzysztof Nienartowicz, Eduard Masana, E. Racero, E. Fraile, Marc Audard, N. Robichon, Luciana Bianchi, G. Gracia-Abril, R. Santoveña, R. Haigron, N. Unger, Jérôme Berthier, Despina Hatzidimitriou, R. Gutiérrez-Sánchez, M. Fabrizio, I. Gonzalez-Santamaria, A. Dapergolas, P. Panuzzo, Benoit Carry, Francesca Figueras, R. Blomme, Elmé Breedt, D. Munoz, Diego Bossini, G. Busso, D. Katz, Simon Hodgkin, Ennio Poretti, N. Brouillet, Marco Castellani, Nicholas Rowell, Arnaud Siebert, M. Romero-Gómez, Shay Zucker, W. van Reeven, A. Kochoska, G. Giuffrida, Eva Sciacca, T. Carlucci, L. M. Sarro, M. I. Carnerero, Amina Helmi, D. Garabato, B. Holl, Michele Bellazzini, L. Rohrbasser, Teresa Antoja, J. Torra, Thomas Hilger, Pedro García-Lario, Gérard Jasniewicz, Enrique Solano, S. G. Baker, W. J. Cooper, F. Royer, S. Accart, George M. Seabroke, João Alves, Emese Plachy, C. Nicolas, Silvio Leccia, N. Cheek, Uwe Lammers, Ramachrisna Teixeira, Techniche Universtât Desden, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lund Observatory, Lund University [Lund], Zentrum für astronomie, Universität Heidelberg [Heidelberg], Department of nuclear medicine, Haukeland University Hospital, University of Bergen (UiB)-University of Bergen (UiB), Merck Serono S.A [Geneva Research Center], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Planetary-system research, Department of Physics, Particle Physics and Astrophysics, Gaia Collaboration, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos Universidad de Barcelona, MDM-2014-0369, Centro de Excelencia Científica Severo Ochoa, Instituto de Ciencias del Cosmos de la Universidad de Barcelona, SEV2015-0493, Deliste, J. B. [0000-0001-5844-9888], Sozzeti, A. [0000-0002-7504-365X], Forderung der wissenschaftlichen Forschung (FWF), Belgian federal Science Policy Office (BELSPO), Hertha Firnberg Programme, Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES), Comite Francais d'Evaluation de la Cooperation Universitaire et Scientifique avec le Bresil (COFECUB), National Natural Science Foundation of China (NSFC), China Scholarship Council (CSC), European Commission (EC), European Research Council (ERC), Hungarian National Research, Development, and Innovation Office (NKFIH), Science Foundation Ireland (SFI), Israel Science Foundation (ISF), Agenzia Spaziale Italiana (ASI), Istituto Nazionale di Astrofisica (INAF), Netherlands Research School for Astronomy (NOVA), Fundacao para a Ciencia e a Tecnologia (FCT), Agencia Estatal de Investigación (AEI), European Space Agency (ESA), Centre National D'Etudes Spatiales (CNES), Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR), Narodowe Centrum Nauki (NCN), Slovenian Research Agency, Swedish National Space Agency (SNSA), United Kingdom Science and Technology Facilities Council (STFC), Universitat de Barcelona (UB), Generalitat de Catalunya, Xunta de Galicia, Universidad de Cantabria, ITA, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Astronomy, and Kapteyn Astronomical Institute
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Data Analysis ,Solar System ,Astronomy ,kinematics and dynamics ,virgo cluster ,Astrophysics ,01 natural sciences ,bar ,Astronomi, astrofysik och kosmologi ,large-magellanic-cloud ,Methods ,Astronomy, Astrophysics and Cosmology ,010303 astronomy & astrophysics ,Physics ,Astrophysics of Galaxies ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrometry ,VIRGO CLUSTER ,Kinematics and Dynamics ,Amplitude ,kinematics ,Physical Sciences ,MILKY-WAY ,astrometry ,Galaxy: kinematics and dynamics ,PROPER MOTION ,Proper motion ,perturbation ,proper motions ,reference systems ,methods: data analysis ,Astrophysics - Astrophysics of Galaxies ,FOS: Physical sciences ,Context (language use) ,proper motion ,Astronomy & Astrophysics ,MASS ,Computer Science::Digital Libraries ,Gravitational potential ,Acceleration ,Settore FIS/05 - Astronomia e Astrofisica ,0103 physical sciences ,data analysis [methods] ,Vector spherical harmonics ,KINEMATICS ,distance ,milky-way ,Science & Technology ,PERTURBATION ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,kinematics and dynamics [Galaxy] ,115 Astronomy, Space science ,Physics::History of Physics ,BAR ,Galaxy ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,DISTANCE ,mass ,LARGE-MAGELLANIC-CLOUD - Abstract
Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions., Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar systembarycentre with respect to the rest frame of the Universe. Apart from being an important scientific result by itself, the acceleration measured in this way is a good quality indicator of the Gaia astrometric solution., Methods. Theeffect of the acceleration was obtained as a part of the general expansion of the vector field of proper motions in vector spherical harmonics (VSH). Various versions of the VSH fit and various subsets of the sources were tried and compared to get the most consistent result and a realistic estimate of its uncertainty. Additional tests with the Gaia astrometric solution were used to get a better idea of the possible systematic errors in the estimate., Results. Our best estimate of the acceleration based on Gaia EDR3 is (2.32 +/- 0.16) x 10(-10) m s(-2) (or 7.33 +/- 0.51 km s(-1) Myr-1) towards alpha = 269.1 degrees +/- 5.4 degrees, delta = -31.6 degrees +/- 4.1 degrees, corresponding to a proper motion amplitude of 5.05 +/- 0.35 mu as yr(-1). This is in good agreement with the acceleration expected from current models of the Galactic gravitational potential. We expect that future Gaia data releases will provide estimates of the acceleration with uncertainties substantially below 0.1 mu as yr(-1).
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- 2020
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48. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - I. Survey description and a first look at G9.62+0.19
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Di Li, Qizhou Zhang, Chao Zhang, Sheng-Li Qin, Feng-Wei Xu, Hyeong-Sik Yun, Feng-Yao Zhu, Paul F. Goldsmith, Shanghuo Li, Yu Wang, Pak Shing Li, Kee-Tae Kim, T. Baug, Neal J. Evans, Isabelle Ristorcelli, Jingwen Wu, Maria Cunningham, Diego Mardones, Ya-Ping Peng, Ken'ichi Tatematsu, Jeong-Eun Lee, Hong-Li Liu, Yuefang Wu, Mika Juvela, Juan Li, Ke Wang, Yong Zhang, Qiu-Yi Luo, Zhiyuan Ren, Anandmayee Tej, Sheng-Yuan Liu, Archana Soam, Sung-ju Kang, X.-W. Liu, Junzhi Wang, Tomoya Hirota, Hee-Weon Yi, Leonardo Bronfman, Zhi-Qiang Shen, Chang Won Lee, L. Viktor Tóth, Namitha Issac, Tie Liu, Guido Garay, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Department of Physics
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stars: kinematics and dynamics ,Library science ,FOS: Physical sciences ,IRAS POINT SOURCES ,7. Clean energy ,01 natural sciences ,ISM: clouds ,COMPETITIVE ACCRETION ,CLUMP IDENTIFICATION ,DENSE MOLECULAR GAS ,Observatory ,0103 physical sciences ,010303 astronomy & astrophysics ,ISM: H ii regions ,Solar and Stellar Astrophysics (astro-ph.SR) ,Physics ,stars: formation ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,CLOUDS ,Astronomy and Astrophysics ,115 Astronomy, Space science ,Astrophysics - Astrophysics of Galaxies ,Chinese academy of sciences ,GALAXIES ,ISM: HII regions ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,MILKY-WAY ,Christian ministry ,COMPLETE SAMPLE ,FRAGMENTATION ,EMISSION - Abstract
The "ATOMS," standing for {\it ALMA Three-millimeter Observations of Massive Star-forming regions}, survey has observed 146 active star forming regions with ALMA Band 3, aiming to systematically investigate the spatial distribution of various dense gas tracers in a large sample of Galactic massive clumps, to study the roles of stellar feedback in star formation, and to characterize filamentary structures inside massive clumps. In this work, the observations, data analysis, and example science of the "ATOMS" survey are presented, using a case study for the G9.62+0.19 complex. Toward this source, some transitions, commonly assumed to trace dense gas, including CS $J = 2-1$, HCO$^+$ $J = 1-0$ and HCN $J = 1-0$, are found to show extended gas emission in low density regions within the clump; less than 25\% of their emission is from dense cores. SO, CH$_3$OH, H$^{13}$CN and HC$_3$N show similar morphologies in their spatial distributions and reveal well the dense cores. Widespread narrow SiO emission is present (over $\sim$1 pc), which may be caused by slow shocks from large--scale colliding flows or H{\sc ii} regions. Stellar feedback from an expanding H{\sc ii} region has greatly reshaped the natal clump, significantly changed the spatial distribution of gas, and may also account for the sequential high-mass star formation in the G9.62+0.19 complex. The ATOMS survey data can be jointly analyzed with other survey data, e.g., "MALT90", "Orion B", "EMPIRE", "ALMA\_IMF", and "ALMAGAL", to deepen our understandings of "dense gas" star formation scaling relations and massive proto-cluster formation., Comment: published on MNRAS
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- 2020
49. Empirical completeness assessment of the Gaia DR2, Pan-STARRS 1 and ASAS-SN-II RR Lyrae catalogues
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Joris De Ridder, Cecilia Mateu, B. Holl, Lorenzo Rimoldini, Mateu Cecilia, Universidad de la República (Uruguay). Facultad de Ciencias. Instituto de Física., Holl Berry, De Ridder Joris, and Rimoldini Lorenzo
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Milky Way ,FOS: Physical sciences ,Astrophysics ,RR Lyrae variable ,Astronomy & Astrophysics ,variables: RR Lyrae [Stars] ,01 natural sciences ,Latitude ,VARIABLE-STARS ,Completeness (order theory) ,0103 physical sciences ,stellar content [Galaxy] ,data analysis [Methods] ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,ALL-SKY VIEW ,Physics ,Science & Technology ,010308 nuclear & particles physics ,Cosmic distance ladder ,Astronomy and Astrophysics ,Catalogues ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Magnitude (astronomy) ,Physical Sciences ,HALO ,MILKY-WAY ,Variable star ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
RR Lyrae stars are an important and widely used tracer of the most ancient populations of our Galaxy, mainly due to their standard candle nature. The availability of large scale surveys of variable stars is allowing us to trace the structure of our entire Galaxy, even in previously inaccessible areas like the Galactic disc. In this work we aim to provide an empirical assessment of the completeness of the three largest RR Lyrae catalogues available: Gaia DR2, PanSTARRS-1 and ASAS-SN-II. Using a joint probabilistic analysis of the three surveys we compute 2D and 3D completeness maps in each survey's full magnitude range. At the bright end (G20deg); ASAS-SN-II has the best completeness at low latitude for RRab and at all latitudes for RRc. At the faint end (G>13), Gaia DR2 is the most complete catalogue for both RR Lyrae types, at any latitude, with median completeness rates of 95% (RRab) and >85% (RRc) outside the ecliptic plane (|��|>25deg). We confirm a high and uniform completeness of PanSTARRS-1 RR Lyrae at 91% (RRab) and 82% (RRc) down to G~18, and provide the first estimate of its completeness at low galactic latitude (|b, 15 pages, 14 figures, 4+10 tables. Accepted for publication at MNRAS. Completeness maps and Python utils to plot and/or recompute them, available at https://github.com/cmateu/rrl_completeness
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- 2020
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50. The Pristine Inner Galaxy Survey (PIGS) I: Tracing the kinematics of metal-poor stars in the Galactic bulge
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Mathias Schultheis, Jeffrey D. Simpson, Zhen Wan, Anke Arentsen, G. F. Thomas, Nicolas F. Martin, K. A. Venn, Rodrigo A. Ibata, K. Youakim, Daniel B. Zucker, Nicolas Longeard, J. I. González Hernández, Vanessa Hill, Julio F. Navarro, Andrea Kunder, R. G. Carlberg, Carmela Lardo, Khyati Malhan, Geraint F. Lewis, Rubén Sánchez-Janssen, David Aguado, Federico Sestito, Else Starkenburg, Arentsen A., Starkenburg E., Martin N.F., Hill V., Ibata R., Kunder A., Schultheis M., Venn K.A., Zucker D.B., Aguado D., Carlberg R., Gonzalez Hernandez J.I., Lardo C., Longeard N., Malhan K., Navarro J.F., Sanchez-Janssen R., Sestito F., Thomas G., Youakim K., Lewis G.F., Simpson J.D., Wan Z., Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France., Centre International de Hautes Etudes Agronomiques Méditerranéennes - Institut Agronomique Méditerranéen de Montpellier (CIHEAM-IAMM), Centre International de Hautes Études Agronomiques Méditerranéennes (CIHEAM), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Toronto, Ecole Polytechnique Fédérale de Lausanne (EPFL), Facultad de Matematicas, Universidad de Murcia, CLRC Daresbury, SFTC, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), and COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)
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photometry ,Milky Way ,Metallicity ,bulge -Galaxy ,kinematics and dynamics -Galaxy ,formation -Galaxy ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Galaxy: Structure ,Galactic halo ,Galaxy: Evolution ,Bulge ,0103 physical sciences ,Galaxy formation and evolution ,structure ,010303 astronomy & astrophysics ,Galaxy: Halo ,halo -Galaxy ,milky-way ,ComputingMilieux_MISCELLANEOUS ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Physics ,Galaxy: Kinematics and dynamic ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] ,stellar populations ,Velocity dispersion ,Astronomy and Astrophysics ,Galaxy: Formation ,argos ,Galaxy: Bulge ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,evolution -Galaxy ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Stars ,[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,galaxy: kinematics and dynamics ,[SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Our Galaxy is known to contain a central boxy/peanut-shaped bulge, yet the importance of a classical, pressure-supported component within the central part of the Milky Way is still being debated. It should be most visible at low metallicity, a regime that has not yet been studied in detail. Using metallicity-sensitive narrow-band photometry, the Pristine Inner Galaxy Survey (PIGS) has collected a large sample of metal-poor ([Fe/H] < -1.0) stars in the inner Galaxy to address this open question. We use PIGS to trace the metal-poor inner Galaxy kinematics as function of metallicity for the first time. We find that the rotational signal decreases with decreasing [Fe/H], until it becomes negligible for the most metal-poor stars. Additionally, the velocity dispersion increases with decreasing metallicity for -3.0 < [Fe/H] < -0.5, with a gradient of -44 $\pm$ 4 km$\,$s$^{-1}\,$dex$^{-1}$. These observations may signal a transition between Galactic components of different metallicities and kinematics, a different mapping onto the boxy/peanut-shaped bulge for former disk stars of different metallicities and/or the secular dynamical and gravitational influence of the bar on the pressure-supported component. Our results provide strong constraints on models that attempt to explain the properties of the inner Galaxy., 5 pages + appendices, accepted to MNRAS Letters
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- 2020
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