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1. Compact and High Excitation Molecular Clumps in the Extended Ultraviolet Disk of M83

Author

Koda, Jin, Combes, Francoise, Rubio, Monica, Andersen, Morten, Bigiel, Frank, de Paz, Armando Gil, Junais, Lee, Amanda M, Meyer, Jennifer Donovan, Morokuma-Matsui, Kana, Yagi, Masafumi, and Zavagno, Annie

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The extended ultraviolet (XUV) disks of nearby galaxies show ongoing massive star formation, but their parental molecular clouds remain mostly undetected despite searches in CO(1-0) and CO(2-1). The recent detection of 23 clouds in the higher excitation transition CO(3-2) within the XUV disk of M83 requires an explanation. We test the hypothesis: the clouds in XUV disks have a clump-envelope structure similar to those in Galactic star-forming clouds, having star-forming dense clumps (or concentrations of multiple clumps) at their centers, which predominantly contribute to the CO(3-2) emission, surrounded by less-dense envelopes, where CO molecules are photo-dissociated due to the low-metallicity environment there. We utilize new high-resolution ALMA CO(3-2) observations of a subset (11) of the 23 clouds in the XUV disk. We confirm the compactness of the CO(3-2)-emitting dense clumps (or their concentrations), finding clump diameters below the spatial resolution of 6-9~pc. This is similar to the size of the dense gas region in the Orion A molecular cloud, the local star-forming cloud with massive star formation. The dense star-forming clumps are common between normal and XUV disks. This may also indicate that once the cloud structure is set, the process of star formation is governed by the cloud internal physics rather than by external triggers. This simple model explains the current observations of the clouds with ongoing massive star formation, although it may require some adjustment, e.g., including an effect of cloud evolution, for a general scenario of star formation in molecular clouds., Comment: A&A accepted; 15 pages, 8 figures - after proof

Published
2024

2. From Bubbles and Filaments to Cores and Disks: Gas Gathering and Growth of Structure Leading to the Formation of Stellar Systems

Author

Pineda, Jaime E., Arzoumanian, Doris, André, Philippe, Friesen, Rachel K., Zavagno, Annie, Clarke, Seamus D., Inoue, Tsuyoshi, Chen, Che-Yu, Lee, Yueh-Ning, Soler, Juan D., and Kuffmeier, Michael

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

The study of the development of structures on multiple scales in the cold interstellar medium has experienced rapid expansion in the past decade, on both the observational and the theoretical front. Spectral line studies at (sub-)millimeter wavelengths over a wide range of physical scales have provided unique probes of the kinematics of dense gas in star-forming regions, and have been complemented by extensive, high dynamic range dust continuum surveys of the column density structure of molecular cloud complexes, while dust polarization maps have highlighted the role of magnetic fields. This has been accompanied by increasingly sophisticated numerical simulations including new physics (e.g., supernova driving, cosmic rays, non-ideal magneto-hydrodynamics, radiation pressure) and new techniques such as zoom-in simulations allowing multi-scale studies. Taken together, these new data have emphasized the anisotropic growth of dense structures on all scales, from giant ISM bubbles driven by stellar feedback on $\sim$50-100 pc scales through parsec-scale molecular filaments down to $<$0.1 pc dense cores and $<$1000 au protostellar disks. Combining observations and theory, we present a coherent picture for the formation and evolution of these structures and synthesize a comprehensive physical scenario for the initial conditions and early stages of star and disk formation., Comment: 42 pages, 20 figures. To appear in Protostars and Planets VII, Editors: Shu-ichiro Inutsuka, Yuri Aikawa, Takayuki Muto, Kengo Tomida, and Motohide Tamura. Small changes to match proofs and the updated format

Published
2022

3. Velocity structure of the 50 pc-long NGC 6334 filamentary cloud: Hints of multiple compressions and their impact on the cloud properties?

Author

Arzoumanian, Doris, Russeil, Delphine, Zavagno, Annie, Chen, Michael Chun-Yuan, André, Philippe, Inutsuka, Shu-ichiro, Misugi, Yoshiaki, Sánchez-Monge, Álvaro, Schilke, Peter, Men'shchikov, Alexander, and Kohno, Mikito

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

[Abridged] The interstellar medium is observed to be organised in filamentary structures, as well as neutral (HI) and ionized (HII) bubbles. The expanding nature of these bubbles makes them shape their surroundings and possibly play a role in the formation and evolution of interstellar filaments. We present APEX $^{13}$CO and C$^{18}$O(2-1) observations of the NGC 6334 molecular cloud. We investigate the gas velocity structure along and across the 50 pc-long cloud and towards 75 identified velocity-coherent-filaments (VCFs). We measure a wealth of velocity gradients along the VCFs. We derive the column density and velocity power spectra of the VCFs. These power spectra are well represented with power laws showing similar slopes for both quantities (with a mean of about -2), albeit some differ by up to a factor of two. The position velocity diagrams perpendicular to three VCFs show the V-shaped velocity pattern, corresponding to a bent structure in velocity space with the filament at the tip of the V surrounded by an extended structure connected to it with a velocity gradient. This velocity structure is qualitatively similar to that resulting from numerical simulations of filament formation from large-scale compression from propagating shock fronts. In addition, the radial profiles perpendicular to these VCFs hint to small-scale internal impacts from neighbouring HII bubbles. The observed opposite curvature in velocity space towards the VCFs points to various origins of large-scale external compressions from propagating HI bubbles. This suggests the plausible importance of multiple HI compressions, separated in space and time, in the formation and evolution of molecular clouds and their star formation history. These latter atomic compressions due to past and distant star formation events are complemented by the impact of HII bubbles from present time and local star formation activity., Comment: Accepted for publication in Astronomy & Astrophysics

Published
2022
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4. Stellar feedback and triggered star formation in the prototypical bubble RCW 120

Author

Luisi, Matteo, Anderson, Loren D., Schneider, Nicola, Simon, Robert, Kabanovic, Slawa, Güsten, Rolf, Zavagno, Annie, Broos, Patrick S., Buchbender, Christof, Guevara, Cristian, Jacobs, Karl, Justen, Matthias, Klein, Bernd, Linville, Dylan, Röllig, Markus, Russeil, Delphine, Stutzki, Jürgen, Tiwari, Maitraiyee, Townsley, Leisa K., and Tielens, Alexander G. G. M.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Radiative and mechanical feedback of massive stars regulates star formation and galaxy evolution. Positive feedback triggers the creation of new stars by collecting dense shells of gas, while negative feedback disrupts star formation by shredding molecular clouds. Although key to understanding star formation, their relative importance is unknown. Here, we report velocity-resolved observations from the SOFIA (Stratospheric Observatory for Infrared Astronomy) legacy program FEEDBACK of the massive star-forming region RCW 120 in the [CII] 1.9-THz fine-structure line, revealing a gas shell expanding at 15 km/s. Complementary APEX (Atacama Pathfinder Experiment) CO J=3-2 345-GHz observations exhibit a ring structure of molecular gas, fragmented into clumps that are actively forming stars. Our observations demonstrate that triggered star formation can occur on much shorter time scales than hitherto thought (<0.15 million years), suggesting that positive feedback operates on short time periods., Comment: 8 Pages, 4 Figures, 1 Table (+16 Page Supplementary Materials with 10 Figures). Published in Science Advances on April 9th, 2021, with free open access to the online article available at https://advances.sciencemag.org/content/7/15/eabe9511

Published
2021
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5. Star Formation, Triggering

Author

Zavagno, Annie, Gargaud, Muriel, editor, Irvine, William M., editor, Amils, Ricardo, editor, Claeys, Philippe, editor, Cleaves, Henderson James, editor, Gerin, Maryvonne, editor, Rouan, Daniel, editor, Spohn, Tilman, editor, Tirard, Stéphane, editor, and Viso, Michel, editor

Published
2023
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6. APEX CO observations towards the photodissociation region of RCW120

Author

Figueira, Miguel, Zavagno, Annie, Bronfman, Leonardo, Russeil, Delphine, Finger, Ricardo, and Schuller, Frédéric

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The edges of ionized (HII) regions are important sites for the formation of (high-mass) stars. Indeed, at least 30% of the galactic high mass star formation is observed there. The radiative and compressive impact of the HII region could induce the star formation at the border following different mechanisms such as the Collect & Collapse (C&C) or the Radiation Driven Implosion (RDI) models and change their properties. We study the properties of two zones located in the Photo Dissociation Region (PDR) of the Galactic HII region RCW120 and discussed them as a function of the physical conditions and young star contents found in both clumps. Using the APEX telescope, we mapped two regions of size 1.5'$\times$1.5' toward the most massive clump of RCW120 hosting young massive sources and toward a clump showing a protrusion inside the HII region and hosting more evolved low-mass sources. The $^{12}$CO($J=3-2$), $^{13}$CO($J=3-2$) and C$^{18}$O($J=3-2$) lines are used to derive the properties and dynamics of these clumps. We discuss their relation with the hosted star-formation. The increase of velocity dispersion and $T_{ex}$ are found toward the center of the maps, where star-formation is observed with Herschel. Furthermore, both regions show supersonic Mach number. No strong evidences have been found concerning the impact of far ultraviolet (FUV) radiation on C$^{18}$O photodissociation. The fragmentation time needed for the C&C to be at work is equivalent to the dynamical age of RCW120 and the properties of region B are in agreement with bright-rimmed clouds. It strengthens the fact that, together with evidences of compression, C&C might be at work at the edges of RCW120. Additionally, the clump located at the eastern part of the PDR is a good candidate of pre-existing clump where star-formation may be induced by the RDI mechanism., Comment: 13 pages, 12 Figures To be published in A&A

Published
2020
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7. Unveiling the importance of magnetic fields in the evolution of dense clumps formed at the waist of bipolar H II regions: a case study on Sh2-201 with JCMT SCUBA-2/POL-2

Author

Eswaraiah, Chakali, Li, Di, Samal, Manash R., Wang, Jia-Wei, Ma, Yuehui, Lai, Shih-Ping, Zavagno, Annie, Ching, Tao-Chung, Liu, Tie, Pattle, Kate, Ward-Thompson, Derek, Pandey, Anil K., and Ojha, Devendra K.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the properties of magnetic fields (B-fields) in two clumps (clump 1 and clump 2), located at the waist of the bipolar H II region Sh2-201, based on JCMT SCUBA-2/POL-2 observations of 850 $\mu$m polarized dust emission. We find that B-fields in the direction of the clumps are bent and compressed, showing bow-like morphologies, which we attribute to the feedback effect of the H II region on the surface of the clumps. Using the modified Davis-Chandrasekhar-Fermi method we estimate B-fields strengths of 266 $\mu$G and 65 $\mu$G for clump 1 and clump 2, respectively. From virial analyses and critical mass ratio estimates, we argue that clump 1 is gravitationally bound and could be undergoing collapse, whereas clump 2 is unbound and stable. We hypothesize that the interplay between thermal pressure imparted by the H II region, B-field morphologies, and the various internal pressures of the clumps (such as magnetic, turbulent, and gas thermal pressure), has the following consequences: (a) formation of clumps at the waist of the H II region; (b) progressive compression and enhancement of the B-fields in the clumps; (c) stronger B-fields will shield the clumps from erosion by the H II region and cause pressure equilibrium between the clumps and the H II region, thereby allowing expanding I-fronts to blow away from the filament ridge, forming bipolar H II regions; and (d) stronger B-fields and turbulence will be able to stabilize the clumps. A study of a larger sample of bipolar H II regions would help to determine whether our hypotheses are widely applicable., Comment: 25 pages, 10 figures, and 4 tables. Accepted for publication in ApJ

Published
2019
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8. The effects of ionization feedback on star formation: A case study of the M16 H II region

Author

Xu, Jin-Long, Zavagno, Annie, Yu, Naiping, Liu, Xiao-Lan, Xu, Ye, Yuan, Jinghua, Zhang, Chuan-Peng, Zhang, Si-Ju, Zhang, Guo-Yin, Ning, Chang-Chun, and Ju, Bing-Gang

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We aim to investigate the impact of the ionized radiation from the M16 HII region on the surrounding molecular cloud and on its hosted star formation. To present comprehensive multi-wavelength observations towards the M16 HII region, we used new CO data and existing infrared, optical, and submillimeter data. The 12CO J=1-0, 13CO J=1-0, and C18O J=1-0 data were obtained with the Purple Mountain Observatory (PMO) 13.7m radio telescope. To trace massive clumps and extract young stellar objects (YSOs) associated with the M16 HII region, we used the ATLASGAL and GLIMPSE I catalogs, respectively. From CO data, we discern a large-scale filament with three velocity components. Because these three components overlap with each other in both velocity and space, the filament may be made of three layers. The M16 ionized gas interacts with the large-scale filament and has reshaped its structure. In the large-scale filament, we find 51 compact cores from the ATLASGAL catalog, 20 of them being quiescent. The mean excitation temperature of these cores is 22.5 K, while this is 22.2 K for the quiescent cores. This high temperature observed for the quiescent cores suggests that the cores may be heated by M16 and do not experience internal heating from sources in the cores. Through the relationship between the mass and radius of these cores, we obtain that 45% of all the cores are massive enough to potentially form massive stars. Compared with the thermal motion, the turbulence created by the nonthermal motion is responsible for the core formation. For the pillars observed towards M16, the H II region may give rise to the strong turbulence., Comment: 18 pages, 12 figures, accepted for publication in A&A

Published
2019
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9. Bipolar H{\sc ii} regions produced by cloud/cloud collisions

Author

Whitworth, Anthony, Lomax, Oliver, Balfour, Scott, Mège, Pierre, Zavagno, Annie, and Deharveng, Lise

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We suggest that Bipolar H{\sc ii} Regions may be the aftermath of collisions between clouds. Such a collision will produce a shock-compressed layer, and a star cluster can then condense out of the dense gas near the centre of the layer. If the clouds are sufficiently massive, the star cluster is likely to contain at least one massive star, which emits ionising radiation, and excites an H{\sc ii} region, which then expands, sweeping up the surrounding neutral gas. Once most of the matter in the clouds has accreted onto the layer, expansion of the H{\sc ii} Region meets little resistance in directions perpendicular to the mid-plane of the layer, and so it expands rapidly to produce two lobes of ionised gas, one on each side of the layer. Conversely, in directions parallel to the mid-plane of the layer, expansion of the H{\sc ii} Region stalls due to the ram-pressure of the gas that continues to fall towards the star cluster from the outer parts of the layer; a ring of dense neutral gas builds up around the waist of the Bipolar H{\sc ii} Region, and may spawn a second generation of star formation. In this paper we present a dimensionless model for the flow of ionised gas in a Bipolar H{\sc ii} Region created according to the above scenario, and predict the characteristics of the resulting freefree continuum and recombination-line emission. This dimensionless model can be scaled to the physical parameters of any particular system. Our intention is that these predictions will be useful in testing the scenario outlined above, and thereby providing indirect support for the role of cloud/cloud collisions in triggering star formation., Comment: 17 pages, 6 figures

Published
2018
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10. ALMA observations of RCW 120 Fragmentation at 0.01pc scale

Author

Figueira, Miguel, Bronfman, Leonardo, Zavagno, Annie, Louvet, Fabien, Lo, Nadia, Finger, Ricardo, and Rodón, Javier

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Little is known about how high-mass stars form. Around 30\% of the young high-mass stars in the Galaxy are observed at the edges of ionized (HII) regions. Therefore these are places of choice to study the earliest stages of high-mass star formation, especially towards the most massive condensations. High-spatial resolution observations in the millimeter range might reveal how these stars form and how they assemble their mass. We want to study the fragmentation process down to the 0.01~pc scale in the most massive condensation observed at the south-western edge of the HII region RCW~120 where the most massive Herschel cores ($\sim$124~$M_{\odot}$ in average) could form high-mass stars. Using ALMA 3~mm continuum observations towards the densest and most massive millimetric condensation (Condensation 1) of RCW~120, we used the getimages and getsources algorithms to extract the sources detected with ALMA and obtained their physical parameters. The fragmentation of the hersche cores is discussed through their Jeans mass to understand the properties of the future stars. We extracted 18 fragments from the ALMA continuum observation at 3~mm towards 8 cores detected with Herschel, whose mass and deconvolved size range from 2~$M_{\odot}$ to 32~$M_{\odot}$ and from 1.6~mpc to 28.8~mpc, respectively. The low degree of fragmentation observed, regarding to the thermal Jeans fragmentation, suggests that the observed fragmentation is inconsistent with ideal gravitational fragmentation and other ingredients such as turbulence or magnetic fields should be added in order to explain it. Finally, the range of fragments' mass indicates that the densest condensation of RCW~120 is a favourable place for the formation of high-mass stars with the presence of a probable UCHII region associated with the 27~$M_{\odot}$ Fragment 1 of Core 2., Comment: 7 pages, 4 figures

Published
2018
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11. High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22

Author

Yuan, Jinghua, Li, Jin-Zeng, Wu, Yuefang, Ellingsen, Simon P., Henkel, Christian, Wang, Ke, Liu, Tie, Liu, Hong-Li, Zavagno, Annie, Ren, Zhiyuan, and Huang, Ya-Fang

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 which is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 $M_\odot$ Myr$^{-1}$, suggesting the hub mass would be doubled in six free-fall times, adding up to $ \sim2 $ Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO$^+$ $ (3-2) $ and $^{13}$CO $ (3-2) $ spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s$^{-1}$ and $ 7.2 \times10^{-4} $ $M_\odot$ yr$^{-1}$, respectively. In clump C1, a hot molecular core (SMA1) is revealed by the SMA observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be $ 11-15 $ $M_\odot$ and it is still growing with an accretion rate of $ 7\times10^{-5} $ $M_\odot$ yr$^{-1}$. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse., Comment: 17 pages, 16 figures 3 tables. and Accepted for publication in ApJ

Published
2017
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12. High-mass Starless Clumps in the inner Galactic Plane: the Sample and Dust Properties

Author

Yuan, Jinghua, Wu, Yuefang, Ellingsen, Simon P., Evans II, Neal J., Henkel, Christian, Wang, Ke, Liu, Hong-Li, Liu, Tie, Li, Jin-Zeng, and Zavagno, Annie

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We report a sample of 463 high-mass starless clump (HMSC) candidates within $-60\deg0.08$ g cm$^{-2}$ could be possible high-mass starless cores. Further investigations toward these HMSCs would undoubtedly shed light on comprehensively understanding the birth of high-mass stars., Comment: 16 pages, 15 figures, and 5 tables. Accepted for publication in ApJS. FITS images for the far-IR to sub-mm data, H2 column density and dust temperature maps of all the HMSC candidates are available at https: //yuanjinghua.github.io/hmscs.html. Codes used for this work are publicly available from https://github.com/yuanjinghua/HMSCs_cat

Published
2017
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13. Herschel observations of the Galactic HII region RCW 79

Author

Liu, Hong-Li, Figueira, Miguel, Zavagno, Annie, Hill, Tracey, Schneider, Nicola, Men'shchikov, Alexander, Russeil, Delphine, Motte, Frederique, Tige, Jeremy, Deharveng, Lise, Anderson, L. D., Li, Jin-Zeng, Wu, Yuefang, Yuan, Jing-Hua, and Huang, Maohai

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Triggered star formation around HII regions could be an important process. The Galactic HII region RCW 79 is a prototypical object for triggered high-mass star formation. We take advantage of Herschel data from the surveys HOBYS, "Evolution of Interstellar Dust", and Hi-Gal to extract compact sources in this region, complemented with archival 2MASS, Spitzer, and WISE data to determine the physical parameters of the sources (e.g., envelope mass, dust temperature, and luminosity) by fitting the spectral energy distribution. We obtained a sample of 50 compact sources, 96% of which are situated in the ionization-compressed layer of cold and dense gas that is characterized by the column density PDF with a double-peaked lognormal distribution. The 50 sources have sizes of 0.1-0.4 pc with a typical value of 0.2 pc, temperatures of 11-26 K, envelope masses of 6-760 $M_\odot$, densities of 0.1-44 $\times$ $10^5$ cm$^{-3}$, and luminosities of 19-12712 $L_\odot$. The sources are classified into 16 class 0, 19 intermediate, and 15 class I objects. Their distribution follows the evolutionary tracks in the diagram of bolometric luminosity versus envelope mass (Lbol-Menv) well. A mass threshold of 140 $M_\odot$, determined from the Lbol-Menv diagram, yields 12 candidate massive dense cores that may form high-mass stars. The core formation efficiency (CFE) for the 8 massive condensations shows an increasing trend of the CFE with density. This suggests that the denser the condensation, the higher the fraction of its mass transformation into dense cores, as previously observed in other high-mass star-forming regions., Comment: Accepted by A&A on 17 January 2017

Published
2017
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14. Interactions of the Infrared bubble N4 with the surroundings

Author

Liu, Hong-Li, Li, Jin-Zeng, Wu, Yuefang, Yuan, Jing-Hua, Liu, Tie, Dubner, G., Paron, S., Ortega, M. E., Molinari, Sergio, Huang, Maohai, Zavagno, Annie, Samal, Manash R., Huang, Ya-Fang, and Zhang, Si-Ju

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The physical mechanisms that induce the transformation of a certain mass of gas in new stars are far from being well understood. Infrared bubbles associated with HII regions have been considered to be good samples of investigating triggered star formation. In this paper we report on the investigation of the dust properties of the infrared bubble N4 around the HII region G11.898+0.747, analyzing its interaction with its surroundings and star formation histories therein, with the aim of determining the possibility of star formation triggered by the expansion of the bubble. Using Herschel PACS and SPIRE images with a wide wavelength coverage, we reveal the dust properties over the entire bubble. Meanwhile, we are able to identify six dust clumps surrounding the bubble, with a mean size of 0.50 pc, temperature of about 22 K, mean column density of 1.7 $\times10^{22}$ cm$^{-2}$, mean volume density of about 4.4 $\times10^{4}$ cm$^{-3}$, and a mean mass of 320 $M_{\odot}$. In addition, from PAH emission seen at 8 $\mu$m, free-free emission detected at 20 cm and a probability density function in special regions, we could identify clear signatures of the influence of the HII region on the surroundings. There are hints of star formation, though further investigation is required to demonstrate that N4 is the triggering source., Comment: Accepted by ApJ (16 pages, 11 figures, 9 tables)

Published
2016
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15. The Milky Way as a Star Formation Engine

Author

Molinari, Sergio, Bally, John, Glover, Simon, Moore, Toby, Noriega-Crespo, Alberto, Plume, René, Testi, Leonardo, Vázquez-Semadeni, Enrique, Zavagno, Annie, Bernard, Jean-Philippe, and Martin, Peter

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The cycling of material from the interstellar medium (ISM) into stars and the return of stellar ejecta into the ISM is the engine that drives the "galactic ecology" in normal spirals, a cornerstone in the formation and evolution of galaxies through cosmic time. Major observational and theoretical challenges need to be addressed in determining the processes responsible for converting the low-density ISM into dense molecular clouds, forming dense filaments and clumps, fragmenting them into stars, OB associations and bound clusters, and characterizing the feedback that limits the rate and efficiency of star formation. This formidable task can be now effectively attacked thanks to the combination of new global-scale surveys of the Milky Way Galactic Plane from infrared to radio wavelengths, offering the possibility of bridging the gap between local and extragalactic star formation studies. The Herschel, Spitzer and WISE mid to far infrared continuum surveys, complemented by analogue surveys from ground-based facilities in the millimetre and radio wavelengths, enables us to measure the Galactic distribution and physical properties of dust on all scales and in all components of the ISM from diffuse clouds to filamentary complexes and tens of thousands of dense clumps. A complementary suite of spectroscopic surveys in various atomic and molecular tracers is providing the chemical fingerprinting of dense clumps and filaments, as well as essential kinematic information to derive distances and thus transform panoramic data into a 3D representation. The latest results emerging from these Galaxy-scale surveys are reviewed. New insights into cloud formation and evolution, filaments and their relationship to channeling gas onto gravitationally-bound clumps, the properties of these clumps, density thresholds for gravitational collapse, and star and cluster formation rates are discussed., Comment: Accepted for publication as a chapter in Protostars and Planets VI, University of Arizona Press (2014), eds. H. Beuther, R. Klessen, C. Dullemond, Th. Henning (minor text revisions, plus updated figure 11)

Published
2014
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16. Dissecting Star-forming regions with the GeMS MCAO instrument: lessons learned for optimal post-processing of WFAO data

Author

Bernard, Ana¨ıs, Neichel, Benoit, Fusco, Thierry, Mugnier, Laurent, Bounissou, Sophie, Samal, Manash, Andersen, Morten, Zavagno, Annie, and Plana, Henri

Subjects
Wide field adaptive optics, data processing, star forming region, photometry, correction of distortions
Abstract

The advent of a new generation of Wide Field AO (WFAO) systems marks the beginning of a new era in high spatial resolution imaging. By using multiple Laser Guide Stars, WFAO significantly increases the field of view of the AOcorrected images, and the fraction of the sky that can benefit from such correction. The newly commissioned Gemini South Multi-Conjugate Adaptive Optics System (GeMS) combined with the infrared camera GSAOI is delivering almost di raction-limited images over a field of   2 arc-minutes across. In this paper, we first present recent observations of the young star-forming region N159W located in the Large Magellanic Cloud. We obtained deep JHKs images from the GeMS/ GSAOI instrument and developed reduction tools, in order to photometrically study the properties of the stellar members of the cluster and to bring new elements to our understanding of the process of massive star formation. However, despite the excellent performance of the GeMS/ GSAOI system, some variable residues are still limiting the correction quality over the field. In particular, GSAOI is severely a ected by distortion that can strongly degrade the resolution when combining multiple frames and can consequently reduce the sensitivity. The accuracy of the distortion correction of an instrument is critical for its use for high- precision astrometry and photometry. In a second part of this paper, we investigate an optimal way to correct for the distortion following an inverse problem approach. The formalism as well as first simulation results are presented.

Published
2015

17. Variation in dust properties in a dense filament of the Taurus molecular complex (L1506)

Author

Ysard, Nathalie, Abergel, Alain, Ristorcelli, Isabelle, Juvela, Mika, Pagani, Laurent, Konyves, Vera, Spencer, Locke, White, Glenn, and Zavagno, Annie

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We observed the L1506 filament, which is located in the Taurus molecular complex, with the Herschel PACS and SPIRE instruments. Our aim is to prove the variation in grain properties along the entire length of the filament. In particular, we want to determine above which gas density this variation arises and what changes in the grain optical properties/size distribution are required. We use the 3D radiative transfer code CRT, coupled to the dust emission and extinction code DustEM, to model the emission and extinction of the dense filament. We test a range of optical properties and size distributions for the grains: dust of the diffuse interstellar medium (interstellar PAHs and amorphous carbons and silicates) and both compact and fluffy aggregates. We find that the grain opacity has to increase across the filament to fit simultaneously the near-IR extinction and Herschel emission profiles of L1506. We interpret this change to be a consequence of the coagulation of dust grains to form fluffy aggregates. Grains similar to those in the diffuse medium have to be present in the outer layers of the cloud, whereas aggregates must prevail above gas densities of a few 1000 H/cm3. This corresponds to line-of-sights with visual extinction in the V band of the order of 2 to 3. The dust opacity at 250 microns is raised by a factor of 1.8 to 2.2, while the grain average size is increased by a factor of 5. These exact numbers depend naturally on the dust model chosen to fit the data. Our findings agree with the constraints given by the study of the gas molecular lines. Using a simple approach, we show that the aggregates may have time to form inside the filament within the cloud lifetime. Our model also characterises the density structure of the filament, showing that the filament width is not constant along L1506 but instead varies by a factor of the order of 4., Comment: accepted for publication in A&A, low resolution figures to match the requirements of arXiv

Published
2013
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19. Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites

Author

Hill, Tracey, Motte, Frederique, Didelon, Pierre, Bontemps, Sylvain, Minier, Vincent, Hennemann, Martin, Schneider, Nicola, Andre, Philippe, Men'shchikov, Alexander, Anderson, Loren D., Arzoumanian, Doris, Bernard, Jean-Philippe, di Francesco, James, Elia, Davide, Giannini, Teresa, Griffin, Matt J., Kirk, Jason, Konyves, Vera, Marston, Anthony P., Martin, Peter, Molinari, Sergio, Luong, Quang Nguyen, Peretto, Nicolas, Pezzuto, Stefano, Roussel, Helene, Sauvage, Marc, Sousbie, Thierry, Testi, Leonardo, Ward-Thompson, Derek, White, Glenn J., Wilson, Christine D., and Zavagno, Annie

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the first Herschel PACS and SPIRE results of the Vela C molecular complex in the far-infrared and submillimetre regimes at 70, 160, 250, 350, and 500 um, spanning the peak of emission of cold prestellar or protostellar cores. Column density and multi-resolution analysis (MRA) differentiates the Vela C complex into five distinct sub-regions. Each sub-region displays differences in their column density and temperature probability distribution functions (PDFs), in particular, the PDFs of the `Centre-Ridge' and `South-Nest' sub-regions appear in stark contrast to each other. The Centre-Ridge displays a bimodal temperature PDF representative of hot gas surrounding the HII region RCW 36 and the cold neighbouring filaments, whilst the South-Nest is dominated by cold filamentary structure. The column density PDF of the Centre-Ridge is flatter than the South-Nest, with a high column density tail, consistent with formation through large-scale flows, and regulation by self-gravity. At small to intermediate scales MRA indicates the Centre-Ridge to be twice as concentrated as the South-Nest, whilst on larger scales, a greater portion of the gas in the South-Nest is dominated by turbulence than in the Centre-Ridge. In Vela C, high-mass stars appear to be preferentially forming in ridges, i.e., dominant high column density filaments., Comment: 7 pages + 2 page figure appendix, 8 Figures (one in the appendix). Accepted by A&A

Published
2011
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20. Calibration of the AKARI Far-Infrared Imaging Fourier Transform Spectrometer

Author

Murakami, Noriko, Kawada, Mitsunobu, Takahashi, Hidenori, Okada, Yoko, Yasuda, Akiko, Ootsubo, Takafumi, Kaneda, Hidehiro, Matsuo, Hiroshi, Baluteau, Jean-Paul, Davis-Imhof, Peter, Gom, Brad G., Naylor, David A., Zavagno, Annie, Yamamura, Issei, Matsuura, Shuji, Shirahata, Mai, Doi, Yasuo, Nakagawa, Takao, and Shibai, Hiroshi

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Far-Infrared Surveyor (FIS) onboard the AKARI satellite has a spectroscopic capability provided by a Fourier transform spectrometer (FIS-FTS). FIS-FTS is the first space-borne imaging FTS dedicated to far-infrared astronomical observations. We describe the calibration process of the FIS-FTS and discuss its accuracy and reliability. The calibration is based on the observational data of bright astronomical sources as well as two instrumental sources. We have compared the FIS-FTS spectra with the spectra obtained from the Long Wavelength Spectrometer (LWS) of the Infrared Space Observatory (ISO) having a similar spectral coverage. The present calibration method accurately reproduces the spectra of several solar system objects having a reliable spectral model. Under this condition the relative uncertainty of the calibration of the continuum is estimated to be $\pm$ 15% for SW, $\pm$ 10% for 70-85 cm^(-1) of LW, and $\pm$ 20% for 60-70 cm^(-1) of LW; and the absolute uncertainty is estimated to be +35/-55% for SW, +35/-55% for 70-85 cm^(-1) of LW, and +40/-60% for 60-70 cm^(-1) of LW. These values are confirmed by comparison with theoretical models and previous observations by the ISO/LWS., Comment: 22 pages, 10 figures

Published
2010
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21. Triggered star formation on the borders of the Galactic HII region RCW 120

Author

Zavagno, Annie, Pomares, Melanie, Deharveng, Lise, Hosokawa, Takashi, Russeil, Delphine, and Caplan, James

Subjects
Astrophysics
Abstract

To investigate the process of star formation triggered by the expansion of an HII region, we present a multi-wavelength analysis of the Galactic HII region RCW 120 and its surroundings. The collect and collapse model predicts that the layer of gas and dust accumulated between the ionization and shock fronts during the expansion of the HII region collapses and forms dense fragments, giving rise to potential sites of massive-star formation. The aim of our study is to look for such massive fragments and massive young stars on the borders of RCW 120. We mapped the RCW 120 region in the cold dust continuum emission at 1.2 mm to search for these fragments. We supplemented this study with the available near- (2MASS) and mid-IR (GLIMPSE) data to locate the IR sources observed towards this region and to analyse their properties. We then compared the observational results with the predictions of Hosokawa & Inutsuka's model (2005, 2006). At 1.2 mm we detected eight fragments towards this region, five located on its borders. The largest fragment has a mass of about 370 Msun. Class I and Class II young stellar objects are detected all over the region, with some observed far from the ionization front. This result emphasises the possible importance distant interactions between the radiation, escaping from the ionized region, and the surrounding medium.

Published
2007
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22. Star Formation, Triggering

Author

Zavagno, Annie, Gargaud, Muriel, editor, Irvine, William M., editor, Amils, Ricardo, editor, Cleaves, Henderson James (Jim), II, editor, Pinti, Daniele L., editor, Quintanilla, José Cernicharo, editor, Rouan, Daniel, editor, Spohn, Tilman, editor, Tirard, Stéphane, editor, and Viso, Michel, editor

Published
2015
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23. Stellar Feedback in the Star Formation-Gas Density Relation: Comparison between Simulations and Observations

Author

Suin, Paolo, Zavagno, Annie, Colman, Tine, Hennebelle, Patrick, Verliat, Antoine, Russeil, Delphine, Suin, Paolo, Zavagno, Annie, Colman, Tine, Hennebelle, Patrick, Verliat, Antoine, and Russeil, Delphine

Abstract

Context. The impact of stellar feedback on the Kennicutt-Schmidt law (KS law), which relates star formation rate (SFR) to surface gas density, is a topic of ongoing debate. The interpretation of individual cloud observations is challenging due to the various processes at play simultaneously and inherent biases. Therefore, a numerical investigation is necessary to understand the role of stellar feedback and identify observable signatures. Aims. We investigate the role of stellar feedback on the KS law, aiming to identify distinct signatures that can be observed and analysed. Methods. We analyse MHD numerical simulations of a $10^4\,M_{\odot}$ cloud evolving under different feedback prescriptions. The set of simulations contains four types of feedback: with only protostellar jets, with ionising radiation from massive stars $(>8\,M_{\odot})$, with both of them and without any stellar feedback. To compare these simulations with the existing observational results, we analyse their evolution by adopting the same techniques applied in observational studies. Then, we simulate how the same analyses would change if the data were affected by typical observational biases. Conclusions. The presence of stellar feedback strongly influences the KS relation and the star formation efficiency per free-fall time ($\epsilon_\mathrm{ff}$). Its impact is primarily governed by its influence on the cloud's structure. Although the $\epsilon_\mathrm{ff}$ measured in our clouds results to be higher than what is usually observed in real clouds, upon applying prescriptions to mimic observational biases we recover good agreement with the expected values. Therefore, we can infer that observations tend to underestimate the total SFR. Moreover, this likely indicates that the physics included in our simulations is sufficient to reproduce the basic mechanisms contributing to set $\epsilon_\mathrm{ff}$., Comment: 16 pages, 13 figures, accepted for publication to A&A

Published
2023

24. ATOMS: ALMA three-millimeter observations of massive star-forming regions – XIII. Ongoing triggered star formation within clump-fed scenario found in the massive (∼1500 M⨀) clump

Author

Zhang, Siju, primary, Wang, Ke, additional, Liu, Tie, additional, Zavagno, Annie, additional, Juvela, Mika, additional, Liu, Hongli, additional, Tej, Anandmayee, additional, Stutz, Amelia M, additional, Li, Shanghuo, additional, Bronfman, Leonardo, additional, Zhang, Qizhou, additional, Goldsmith, Paul F, additional, Lee, Chang Won, additional, Vázquez-Semadeni, Enrique, additional, Tatematsu, Ken’ichi, additional, Jiao, Wenyu, additional, Xu, Fengwei, additional, Wang, Chao, additional, and Zhou, Jian-Wen, additional

Published
2023
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25. The Next Generation of High-Mass Stars and Clusters Traced by ATLASGAL

Author

Schuller, Frédéric, Menten, Karl M., Wyrowski, Friedrich, Contreras, Yanett, Csengeri, Timea, Urquhart, James S., Wienen, Marion, Beuther, Henrik, Bontemps, Sylvain, Bronfman, Leonardo, Deharveng, Lise, Henning, Thomas, Walmsley, Malcolm, Zavagno, Annie, Stamatellos, Dimitris, editor, Goodwin, Simon, editor, and Ward-Thompson, Derek, editor

Published
2014
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26. Segmentation of the Galactic ISM Filaments using Deep Learning and Hi-GAL Catalogue

Author

BENSAID Siouar, ZAVAGNO Annie, and DUPÉ François Xavier

Subjects
ISM, filaments segmentation, Hi-GAL catalogue, AI, UNet, Deep Learning, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Understanding star formation is key to understand galaxy evolution. Observations collected in the Herschel Infrared Galactic plane Survey (Hi-GAL) revealed the ubiquitous presence of filamentary structures in the Galactic Plane. Filaments host star formation. Therefore, it is very interesting to study them and analyze the environment effect on their life cycle. A first step in understanding filaments consists in detecting them in the Galactic Plane. Detection algorithms based on standard image processing techniques present several limitations. Taking into consideration the drastic progress in Artificial Intelligence (AI), along with the data abundance about filaments, we propose to explore filament segmentation using Deep Learning (DL) framework. In this paper, we use state-of-the-art image segmentation in DL, U-Net, to segment filaments in all the Galactic Plane, in H2 column density images of the Galactic Plane obtained with Herschel Hi-GAL data. The used ground truth consists in the Hi-GAL filament catalogue provided by Schisano et al. Obtained results reveal more structures than provided in the catalogue, which makes AI-based methods very promising for such application.

Published
2022
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28. ATOMS: ALMA three-millimeter observations of massive star-forming regions – XIII. Ongoing triggered star formation within clump-fed scenario found in the massive (∼1500 M⨀) clump.

Author

Zhang, Siju, Wang, Ke, Liu, Tie, Zavagno, Annie, Juvela, Mika, Liu, Hongli, Tej, Anandmayee, Stutz, Amelia M, Li, Shanghuo, Bronfman, Leonardo, Zhang, Qizhou, Goldsmith, Paul F, Lee, Chang Won, Vázquez-Semadeni, Enrique, Tatematsu, Ken'ichi, Jiao, Wenyu, Xu, Fengwei, Wang, Chao, and Zhou, Jian-Wen

Subjects
STAR formation, SUPERGIANT stars, IONIZED gases, IONIZING radiation, GAS flow, PROTOSTARS
Abstract

Whether ionization feedback triggers the formation of massive stars is highly debated. Using ALMA 3-mm observations with a spatial resolution of ∼0.05 pc and a mass sensitivity of 1.1  |$\rm M_\odot$|  per beam at 20 K, we investigate the star formation and gas flow structures within the ionizing feedback-driven structure, a clump-scale massive (≳ 1500  |$\rm M_\odot$|⁠) bright-rimmed cloud (BRC) associated with IRAS 18290–0924. This BRC is bound only if external compression from ionized gas is considered. A small-scale (≲ 1 pc) age sequence along the direction of ionizing radiation is revealed for the embedded cores and protostars, which suggests triggered star formation via radiation-driven implosion (RDI). Furthermore, filamentary gas structures converge towards the cores located in the BRC's centre, indicating that these filaments are fueling mass towards cores. The local core-scale mass infall rate derived from H13CO+  J  = 1 − 0 blue profile is of the same order of magnitude as the filamentary mass inflow rate, approximately 1  |$\rm M_\odot$|  kyr−1. A photodissociation region (PDR) covering the irradiated clump surface is detected in several molecules, such as CCH, HCO+, and CS whereas the spatial distribution stratification of these molecules is indistinct. CCH spectra of the PDR possibly indicate a photoevaporation flow leaving the clump surface with a projected velocity of ∼2 km s−1. Our new observations show that RDI accompanied by a clump-fed process is operating in this massive BRC. Whether this combined process works in other massive BRCs is worth exploring with dedicated surveys. [ABSTRACT FROM AUTHOR]

Published
2023
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29. Velocity structure of the 50 pc long NGC 6334 filamentary cloud

Author

Arzoumanian, Doris, primary, Russeil, Delphine, additional, Zavagno, Annie, additional, Chun-Yuan Chen, Michael, additional, André, Philippe, additional, Inutsuka, Shu-ichiro, additional, Misugi, Yoshiaki, additional, Sánchez-Monge, Álvaro, additional, Schilke, Peter, additional, Men’shchikov, Alexander, additional, and Kohno, Mikito, additional

Published
2022
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30. The Next Generation of High-Mass Stars and Clusters Traced by ATLASGAL

Author

Schuller, Frédéric, primary, Menten, Karl M., additional, Wyrowski, Friedrich, additional, Contreras, Yanett, additional, Csengeri, Timea, additional, Urquhart, James S., additional, Wienen, Marion, additional, Beuther, Henrik, additional, Bontemps, Sylvain, additional, Bronfman, Leonardo, additional, Deharveng, Lise, additional, Henning, Thomas, additional, Walmsley, Malcolm, additional, and Zavagno, Annie, additional

Published
2014
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32. VizieR Online Data Catalog: Probing the ISF in Orion A with ArTeMiS (Schuller+, 2021)

Author

Schuller, F., André, P., Shimajiri, Y., Zavagno, Annie, Peretto, N., Arzoumanian, D., Csengeri, T., Koenyves, V., Palmeirim, P., Pezzuto, S., Rigby, A., Roussel, H., Ajeddig, H., Dumaye, L., Gallais, P., Le Pennec, J., Martignac, J., Mattern, M., Revéret, V., Rodriguez, L., Talvard, M., Max-Planck-Institut für Radioastronomie (MPIFR), 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), 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), Cardiff University, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), FEMIS 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), Universidade do Porto = University of Porto, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Solar Influences Data Analysis Center [Brussels] (SIDC), and Royal Observatory of Belgium [Brussels] (ROB)

Subjects
Interstellar medium, [SDU]Sciences of the Universe [physics], Molecular clouds, ComputingMilieux_MISCELLANEOUS
Abstract

voi; International audience

Published
2021

33. VizieR Online Data Catalog: Polarization measurements of S201 with JCMT (Eswaraiah+, 2020)

Author

Eswaraiah, C., Li, Di, Samal, M.~r., Wang, J. -W., Ma, Y., Lai, S. -P., Zavagno, Annie, Ching, T. -C., Liu, T., Pattle, K., Ward-Thompson, D., Pandey, A.~k., Ojha, D.~k., University of Alberta, 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), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], and University of Central Lancashire [Preston] (UCLAN)

Subjects
Interstellar medium, [SDU]Sciences of the Universe [physics], Magnetic fields, Polarization, H II regions, Optical
Abstract

International audience; Dust continuum polarization observations have been conducted using the POL-2 polarimeter installed on the SCUBA-2 camera (hereafter SCUBAPOL2) at the James Clerk Maxwell Telescope (JCMT), a 15m single-dish submillimeter observatory located on the summit of Maunakea in Hawaii, USA. POL-2 observations of the S201 region (project code: M17BP041; PI: Eswaraiah Chakali) were carried out on 2017 November 18 using the POL-2 DAISY mapping mode. Three sets of observations were acquired under JCMT Band 1 weather conditions, during which the atmospheric optical depth at 225GHz, \tau\225, was 0.03. Each set was observed for 30 minutes, resulting in a total integration time of \raisebox-0.5ex~1.5hr. \\\\(1 data file).

Published
2021

34. H II regions and high-mass starless clump candidates

Author

Zhang, S., Zavagno, Annie, López-Sepulcre, A., Liu, H., Louvet, F., Figueira, M., Russeil, D., Wu, Y., Yuan, J., Pillai, T. G. S., 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 de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), 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), Centro de Matemática e Aplicações Fundamentais (CMAF), Universidade de Lisboa (ULISBOA), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), 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), Universidade de Lisboa = University of Lisbon (ULISBOA), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
stars: massive, HII regions, stars: formation, techniques: interferometric, ISM: structure, submillimeter: ISM, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Context. The ionization feedback from H II regions modifies the properties of high-mass starless clumps (HMSCs, of several hundred to a few thousand solar masses with a typical size of 0.1–1 pc), such as dust temperature and turbulence, on the clump scale. The question of whether the presence of H II regions modifies the core-scale (~0.025 pc) fragmentation and star formation in HMSCs remains to be explored.Aims. We aim to investigate the difference of 0.025 pc-scale fragmentation between candidate HMSCs that are strongly impacted by H II regions and less disturbed ones. We also search for evidence of mass shaping and induced star formation in the impacted candidate HMSCs.Methods. Using the ALMA 1.3 mm continuum, with a typical angular resolution of 1.3′′, we imaged eight candidate HMSCs, including four impacted by H II regions and another four situated in the quiet environment. The less-impacted candidate HMSCs are selected on the basis of their similar mass and distance compared to the impacted ones to avoid any possible bias linked to these parameters. We carried out a comparison between the two types of candidate HMSCs. We used multi-wavelength data to analyze the interaction between H II regions and the impacted candidate HMSCs.Results. A total of 51 cores were detected in eight clumps, with three to nine cores for each clump. Within our limited sample, we did not find a clear difference in the ~0.025 pc-scale fragmentation between impacted and non-impacted candidate HMSCs, even though H II regions seem to affect the spatial distribution of the fragmented cores. Both types of candidate HMSCs present a thermal fragmentation with two-level hierarchical features at the clump thermal Jeans length λJ,clumpth and 0.3λJ,clumpth. The ALMA emission morphology of the impacted candidate HMSCs AGAL010.214-00.306 and AGAL018.931-00.029 sheds light on the capacities of H II regions to shape gas and dust in their surroundings and possibly to trigger star formation at ~0.025 pc-scale in candidate HMSCs.Conclusions. The fragmentation at ~0.025 pc scale for both types of candidate HMSCs is likely to be thermal-dominant, meanwhile H II regions probably have the capacity to assist in the formation of dense structures in the impacted candidate HMSCs. Future ALMA imaging surveys covering a large number of impacted candidate HMSCs with high turbulence levels are needed to confirm the trend of fragmentation indicated in this study.

Published
2021

35. SPHERE+: Imaging young Jupiters down to the snowline

Author

Augereau, J. -C., Baudino, J. -L., Beuzit, J. -L., Bouret, J. -C., Desert, J. -M., Delisle, J. -B., Orazi, V. D, Gonzalez, J. -F., Lagrange, A. -M., Coroller, H. Le, Arena, G. Muro, Diaye, M. N, Sauvage, J. -F., Schmid, H. -M., Boccaletti, A., Chauvin, G., Mouillet, D., Absil, O., Allard, F., Antoniucci, S., Augereau, J.-C, Barge, P., Baruffolo, A., Baudino, J.-L, Baudoz, P., Beaulieu, M., Benisty, M., Beuzit, J.-L, Bianco, A., Biller, B., Bonavita, B., Bonnefoy, M., Bos, S., Bouret, J.-C, Brandner, W., Buchschache, N., Carry, B., Cantalloube, F., Cascone, E., Carlotti, A., Charnay, B., Chiavassa, A., Choquet, E., Clenet, Y., Crida, A., De Boer, J., De Caprio, V., Desidera, S., Desert, J.-M, Delisle, J.-B, Delorme, P., Dohlen, K., Doelman, D., Dominik, C., D'orazi, V, Dougados, C., Douté, S., Fedele, D., Feldt, M., Ferreira, F., Fontanive, C., Fusco, T., Galicher, R., Garufi, A., Gendron, E., Ghedina, A., Ginski, C., Gonzalez, J.-F, Gratadour, D., Gratton, R., Guillot, T., Haffert, S., Hagelberg, J., Henning, T., Huby, E., Janson, M., Kamp, I., Keller, C. U., Kenworthy, M., Kervella, P., Kral, Q., Kuhn, J., Lagadec, E., Laibe, G., Langlois, M., Lagrange, A.-M, Launhardt, R., Leboulleux, L., Le Coroller, H, Causi, G. Li, Loupias, M., Maire, A. L., Marleau, G., Martinache, F., Martinez, P., Mary, D., Mattioli, M., Mazoyer, J., Meheut, H., Ménard, F., Mesa, D., Meunier, N., Miguel, Y., Milli, J., Min, M., Molliere, P., Mordasini, C., Moretto, G., Mugnier, L., Muro Arena, G, Nardetto, N., N'Diaye, M, Nesvadba, N., Pedichini, F., Pinilla, P., Por, E., Potier, A., Quanz, S., Rameau, J., Roelfsema, R., Rouan, D., Rigliaco, E., Salasnich, B., Samland, M., Sauvage, J.-F, Schmid, H.-M, Segransan, D., Snellen, I., Snik, F., Soulez, F., Stadler, E., Stam, D., Tallon, M., Thebault, P., Thiebaut, E., Tschudi, C., Udry, S., van Holstein, R., Vernazza, P, Vidal, F., Vigan, A., Waters, R., Wildi, F., Willson, M., Zanutta, A., Zavagno, Annie, Zurlo, A., 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), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], 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), Observatoire de la Cte d’Azur, 96 Boulevard de l’Observatoire, Nice, 06300, France, Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Département de Recherche sur la Fusion Contrôlée (DRFC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Department of Biochemistry and Molecular Biology, Mayo Clinic, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Université Côte d'Azur (UCA), University of Arizona, 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 Paris Cité (UPCité), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), NOVA Optical Infrared Instrumentation Group, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS 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), SRON Netherlands Institute for Space Research (SRON), Croissance et propriétés de systèmes hybrides en couches minces (INSP-E8), Institut des Nanosciences de Paris (INSP), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Unité de recherche d'Économie et Sociologie Rurales (ESR), Institut National de la Recherche Agronomique (INRA), INAF - Osservatorio Astronomico di Roma (OAR), Universität Greifswald - University of Greifswald, European Southern Observatory [Santiago] (ESO), Immunopathologie et chimie thérapeutique (ICT), Institut de biologie moléculaire et cellulaire (IBMC), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, INAF - Osservatorio Astronomico di Capodimonte (OAC), Hôpital Cochin [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), DOTA, ONERA, Université Paris Saclay [Palaiseau], Department of Astronomy, Stockholm University, Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Sterrewacht Leiden, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-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 Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), 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), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Universiteit Leiden

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

SPHERE (Beuzit et al,. 2019) has now been in operation at the VLT for more than 5 years, demonstrating a high level of performance. SPHERE has produced outstanding results using a variety of operating modes, primarily in the field of direct imaging of exoplanetary systems, focusing on exoplanets as point sources and circumstellar disks as extended objects. The achievements obtained thus far with SPHERE (~200 refereed publications) in different areas (exoplanets, disks, solar system, stellar physics...) have motivated a large consortium to propose an even more ambitious set of science cases, and its corresponding technical implementation in the form of an upgrade. The SPHERE+ project capitalizes on the expertise and lessons learned from SPHERE to push high contrast imaging performance to its limits on the VLT 8m-telescope. The scientific program of SPHERE+ described in this document will open a new and compelling scientific window for the upcoming decade in strong synergy with ground-based facilities (VLT/I, ELT, ALMA, and SKA) and space missions (Gaia, JWST, PLATO and WFIRST). While SPHERE has sampled the outer parts of planetary systems beyond a few tens of AU, SPHERE+ will dig into the inner regions around stars to reveal and characterize by mean of spectroscopy the giant planet population down to the snow line. Building on SPHERE's scientific heritage and resounding success, SPHERE+ will be a dedicated survey instrument which will strengthen the leadership of ESO and the European community in the very competitive field of direct imaging of exoplanetary systems. With enhanced capabilities, it will enable an even broader diversity of science cases including the study of the solar system, the birth and death of stars and the exploration of the inner regions of active galactic nuclei., White paper submitted to ESO on Feb. 20th, 2020

Published
2020

36. Stellar feedback and triggered star formation in the prototypical bubble RCW 120

Author

Luisi, Matteo, primary, Anderson, Loren D., additional, Schneider, Nicola, additional, Simon, Robert, additional, Kabanovic, Slawa, additional, Güsten, Rolf, additional, Zavagno, Annie, additional, Broos, Patrick S., additional, Buchbender, Christof, additional, Guevara, Cristian, additional, Jacobs, Karl, additional, Justen, Matthias, additional, Klein, Bernd, additional, Linville, Dylan, additional, Röllig, Markus, additional, Russeil, Delphine, additional, Stutzki, Jürgen, additional, Tiwari, Maitraiyee, additional, Townsley, Leisa K., additional, and Tielens, Alexander G. G. M., additional

Published
2021
Full Text
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37. VizieR Online Data Catalog: HMSCs classification and physical parameters (Zhang+, 2020)

Author

Zhang, S., Zavagno, Annie, Yuan, J., Liu, H., Figueira, M., Russeil, D., Schuller, F., Marsh, K.~a., Wu, Y., Systèmes de Référence Temps Espace (SYRTE), 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), 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), Rice University [Houston], Centro de Matemática e Aplicações Fundamentais (CMAF), Universidade de Lisboa = University of Lisbon (ULISBOA), Max-Planck-Institut für Radioastronomie (MPIFR), Institute of Applied Physics and Computational Mathematics - IACM (Beijing, China)), and Chinese Academy of Sciences [Beijing] (CAS)

Subjects
Associations: stellar, Interstellar medium, [SDU]Sciences of the Universe [physics], H II regions, Millimetric/submm sources
Abstract

This table (Table 4 in the paper) consists of the basic properties of high-mass starless clump candidates that are updated by this work. \\\\(1 data file).

Published
2020

38. VizieR Online Data Catalog: Accretion history of massive stars (Peretto+, 2020)

Author

Peretto, N., Rigby, A., André, P., Könyves, V., Fuller, G., Zavagno, Annie, Schuller, F., Arzoumanian, D., Bontemps, S., Csengeri, T., Didelon, P., Duarte-Cabral, A., Palmeirim, P., Pezzuto, S., Revéret, V., Roussel, H., Shimajiri, Y., Cardiff University, 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), Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], 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), Max-Planck-Institut für Radioastronomie (MPIFR), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), FORMATION STELLAIRE 2020, 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), FEMIS 2021, School of Physics and Astronomy [Cardiff], Universidade do Porto = University of Porto, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and 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)

Subjects
[SDU]Sciences of the Universe [physics], Molecular clouds, Photometry: millimetric/submm, Infrared sources, Stars: masses
Abstract

This table presents the properties of each of 203 compact ArTeMiS sources identified in the images analysed in the paper. These sources have been identified across 5 fields: SDC326, SDC328, SDC340, SDC343, SDC345. \\\\(1 data file).

Published
2020

39. H II regions and high-mass starless clump candidates

Author

Zhang, S., Zavagno, Annie, Yuan, J., Liu, H., Figueira, M., Russeil, D., Schuller, F., Marsh, K. A., Wu, Y., College of Aerospace Science and Engineering, National University of Defense Technology [China], 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), School of Electrical Engineering and Telecommunications (UNSW), University of New South Wales [Sydney] (UNSW), College of Urban and Environmental Sciences [Beijing], Peking University [Beijing], Max-Planck-Institut für Radioastronomie (MPIFR), and Plant & Food Research

Subjects
stars: formation, submillimeter: ISM, H II regions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Context. The role of ionization feedback on high-mass (>8 M⊙) star formation is still highly debated. Questions remain concerning the presence of nearby H II regions changes the properties of early high-mass star formation and whether H II regions promote or inhibit the formation of high-mass stars.Aims. To characterize the role of H II regions on the formation of high-mass stars, we study the properties of a sample of candidates high-mass starless clumps (HMSCs), of which about 90% have masses larger than 100 M⊙. These high-mass objects probably represent the earliest stages of high-mass star formation; we search if (and how) their properties are modified by the presence of an H II region.Methods. We took advantage of the recently published catalog of HMSC candidates. By cross matching the HMSCs and H II regions, we classified HMSCs into three categories: (1) the HMSCs associated with H II regions both in the position in the projected plane of the sky and in velocity; (2) HMSCs associated in the plane of the sky, but not in velocity; and (3) HMSCs far away from any H II regions in the projected sky plane. We carried out comparisons between associated and nonassociated HMSCs based on statistical analyses of multiwavelength data from infrared to radio.Results. We show that there are systematic differences of the properties of HMSCs in different environments. Statistical analyses suggest that HMSCs associated with H II regions are warmer, more luminous, more centrally-peaked and turbulent. We also clearly show, for the first time, that the ratio of bolometric luminosity to envelope mass of HMSCs (L∕M) could not be a reliable evolutionary probe for early massive star formation due to the external heating effects of the H II regions.Conclusions. We show HMSCs associated with H II regions present statistically significant differences from HMSCs far away from H II regions, especially for dust temperature and L∕M. More centrally peaked and turbulent properties of HMSCs associated with H II regions may promote the formation of high-mass stars by limiting fragmentation. High-resolution interferometric surveys toward HMSCs are crucial to reveal how H II regions impact the star formation process inside HMSCs.

Published
2020

40. VizieR Online Data Catalog: Distance of HiGAL sources (Mege+, 2021)

Author

Mège, P., Russeil, D., Zavagno, Annie, Elia, D., Molinari, S., Brunt, C.~m., Butora, R., Cambresy, L., Di, Giorgio A.~m., Fenouillet, T., Fukui, Y., Lambert, J.~c., Makai, Z., Merello, M., Meunier, J.~c., Molinaro, M., Moreau, C., Pezzuto, S., Poulin, Y., Schisano, E., Schuller, F., 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), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), 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), Department of Astrophysics [Nagoya], Nagoya University, West Virginia University [Morgantown], Departamento de Astronomia (DAS), INAF - Osservatorio Astronomico di Trieste (OAT), Environnement, Ville, Société (EVS), École normale supérieure de Lyon (ENS de Lyon)-École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Université Lumière - Lyon 2 (UL2)-Université Jean Moulin - Lyon 3 (UJML), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-École Nationale des Travaux Publics de l'État (ENTPE)-École nationale supérieure d'architecture de Lyon (ENSAL)-Centre National de la Recherche Scientifique (CNRS), and Max-Planck-Institut für Radioastronomie (MPIFR)

Subjects
Milky Way, Radial velocities, [SDU]Sciences of the Universe [physics], Molecular clouds, Stars: distances
Abstract

Velocity and Distance of HiGAL sources. \\\\(2 data files).

Published
2020

41. VizieR Online Data Catalog: Astrometric parameters for 135 OB stars (Russeil+, 2020)

Author

Russeil, D., Zavagno, Annie, Nguyen, A., Figueira, M., Adami, C., Bouret, J.~c., Beaussier, Catherine, 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), Application des ultrasons à la thérapie (LabTAU), Centre Léon Bérard [Lyon]-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM), Centro de Matemática e Aplicações Fundamentais (CMAF), and Universidade de Lisboa = University of Lisbon (ULISBOA)

Subjects
[SDU] Sciences of the Universe [physics], Stars: OB, [SDU]Sciences of the Universe [physics], H II regions, Parallaxes: trigonometric, Proper motions, YSOs
Abstract

Astrometric information of the 135 spectroscopic OB stars in the regions NGC 6334 and NGC 6357. \\\\For each star spectral type, equatorial coordinates, V and G magnitudes, GAIA identifier, astrometric data, derived distance and tranverse velocity components are given. \\\\(1 data file).

Published
2020

42. The role of Galactic H II regions in the formation of filaments

Author

ZAVAGNO, Annie, ANDRÉ, Ph., SCHULLER, F., PERETTO, N., SHIMAJIRI, Y., ARZOUMANIAN, D., CSENGERI, T., FIGUEIRA, M., FULLER, G. A., KÖNYVES, V., MEN’SHCHIKOV, A., PALMEIRIM, P., ROUSSEL, H., RUSSEIL, D., SCHNEIDER, N., ZHANG, S., 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), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), 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), Leibniz-Institut für Astrophysik Potsdam (AIP), School of Physics and Astronomy [Cardiff], Cardiff University, Kagoshima University, Instituto de Astrofísica e Ciências do Espaço (IASTRO), 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), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University Hospital of Cologne [Cologne], Supports from the French national programs on stellar and ISM physics (PNPS and PCMI)., Funding from the European Union’s Horizon 2020 research and innovation programmeunder grant agreement No 730562 [RadioNet]., ANR-16-CE92-0035,GENESIS,GENeration et Evolution des Structures du milieu InterStellaire(2016), ANR-11-BS56-0010,STARFICH,Vers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel(2011), ANR-05-BLAN-0215,ARTEMIS,ARchitectures de bolomètres pour des TElescopes à grand champ de vue dans le domaine sub-MIllimétrique au Sol(2005), ANR-11-LABX-0013,FOCUS,Des détecteurs pour Observer l'Univers(2011), European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), and 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 de Paris (UP)

Subjects
stars: formation, ISM: individual objects: RCW 120, submillimeter: ISM, H II regions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

This research has made use of data from the Herschel HOBYS project (http://hobys-herschel.cea.fr). HOBYS is a Herschel Key Project jointly carried out by SPIRE Specialist Astronomy Group 3 (SAG3), scientists of the LAM laboratory in Marseille, and scientists of the Herschel Science Center (HSC).; International audience; Context. Massive stars and their associated ionized (H II) regions could play a key role in the formation and evolution of filaments that host star formation. However, the properties of filaments that interact with H II regions are still poorly known.Aims. To investigate the impact of H II regions on the formation of filaments, we imaged the Galactic H II region RCW 120 and its surroundings where active star formation takes place and where the role of ionization feedback on the star formation process has already been studied.Methods. We used the large-format bolometer camera ArTéMiS on the APEX telescope and combined the high-resolution ArTéMiS data at 350 and 450 μm with Herschel-SPIRE/HOBYS data at 350 and 500 μm to ensure good sensitivity to a broad range of spatial scales. This allowed us to study the dense gas distribution around RCW 120 with a resolution of 8′′ or 0.05 pc at a distance of 1.34 kpc.Results. Our study allows us to trace the median radial intensity profile of the dense shell of RCW 120. This profile is asymmetric, indicating a clear compression from the H II region on the inner part of the shell. The profile is observed to be similarly asymmetric on both lateral sides of the shell, indicating a homogeneous compression over the surface. On the contrary, the profile analysis of a radial filament associated with the shell, but located outside of it, reveals a symmetric profile, suggesting that the compression from the ionized region is limited to the dense shell. The mean intensity profile of the internal part of the shell is well fitted by a Plummer-like profile with a deconvolved Gaussian full width at half maximum of 0.09 pc, as observed for filaments in low-mass star-forming regions.Conclusions. Using ArTéMiS data combined with Herschel-SPIRE data, we found evidence for compression from the inner part of the RCW 120 ionized region on the surrounding dense shell. This compression is accompanied with a significant (factor 5) increase of the local column density. This study suggests that compression exerted by H II regions may play a key role in the formation of filaments and may further act on their hosted star formation. ArTéMiS data also suggest that RCW 120 might be a 3D ring, rather than a spherical structure.

Published
2020

43. Unveiling the Importance of Magnetic Fields in the Evolution of Dense Clumps Formed at the Waist of Bipolar H ii Regions: A Case Study of Sh 2-201 with JCMT SCUBA-2/POL-2

Author

Eswaraiah, Chakali, Li, Di, Samal, Manash R., Wang, Jia-Wei, Ma, Yuehui, Lai, Shih-Ping, Zavagno, Annie, Ching, Tao-Chung, Liu, Tie, Pattle, Kate, Ward-Thompson, Derek, Pandey, Anil K., Ojha, Devendra K., Eswaraiah, Chakali, Li, Di, Samal, Manash R., Wang, Jia-Wei, Ma, Yuehui, Lai, Shih-Ping, Zavagno, Annie, Ching, Tao-Chung, Liu, Tie, Pattle, Kate, Ward-Thompson, Derek, Pandey, Anil K., and Ojha, Devendra K.

Abstract

We present the properties of magnetic fields (B fields) in two clumps (clump 1 and clump 2), located at the waist of the bipolar H ii region Sh 2-201, based on James Clerk Maxwell Telescope SCUBA-2/POL-2 observations of 850 μm polarized dust emission. We find that B fields in the direction of the clumps are bent and compressed, showing bow-like morphologies, which we attribute to the feedback effect of the H ii region on the surface of the clumps. Using the modified Davis–Chandrasekhar–Fermi method, we estimate B-field strengths of 266 and 65 μG for clump 1 and clump 2, respectively. From virial analyses and critical mass ratio estimates, we argue that clump 1 is gravitationally bound and could be undergoing collapse, whereas clump 2 is unbound and stable. We hypothesize that the interplay of the thermal pressure imparted by the H ii region, the B-field morphologies, and the various internal pressures of the clumps (such as magnetic, turbulent, and gas thermal pressures) has the following consequences: (a) formation of clumps at the waist of the H ii region; (b) progressive compression and enhancement of the B fields in the clumps; (c) stronger B fields that will shield the clumps from erosion by the H ii region and cause pressure equilibrium between the clumps and the H ii region, thereby allowing expanding ionization fronts to blow away from the filament ridge, forming bipolar H ii regions; and (d) stronger B fields and turbulence that will be able to stabilize the clumps. A study of a larger sample of bipolar H ii regions would help to determine whether our hypotheses are widely applicable.

Published
2020

45. Unveiling the Importance of Magnetic Fields in the Evolution of Dense Clumps Formed at the Waist of Bipolar H ii Regions: A Case Study of Sh 2-201 with JCMT SCUBA-2/POL-2

Author

Eswaraiah, Chakali, primary, Li, Di, additional, Samal, Manash R., additional, Wang, Jia-Wei, additional, Ma, Yuehui, additional, Lai, Shih-Ping, additional, Zavagno, Annie, additional, Ching, Tao-Chung, additional, Liu, Tie, additional, Pattle, Kate, additional, Ward-Thompson, Derek, additional, Pandey, Anil K., additional, and Ojha, Devendra K., additional

Published
2020
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46. FRAGMENTATION OF MASSIVE CORES TOWARD THE GALACTIC Hii REGION RCW 120 OBSERVED WITH ALMA

Author

Figueira, M., Zavagno, Annie, Bronfman, L., National Centre for Nuclear Research [Otwock], Narodowe Centrum Badań Jądrowych (NCBJ), 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), Departamento de Astronomia (DAS), Société Francaise d’Astronomie et d’Astrophysique (SF2A), P. Di Matteo, O. Creevey, A. Crida, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Beaussier, Catherine

Subjects
[SDU] Sciences of the Universe [physics], high-mass star, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], fragmentation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Hii region, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; Feedback from high-mass stars (stellar winds, radiation and photoionization pressure, supernova explosions) can strongly modify the surrounding cloud. As a result, the next generation of stars is affected and can present different physical properties. Using ALMA interferometric observations, we characterized the fragmentation occurring inside the massive cores previously detected with Herschel and being good candidates for high-mass star formation. Most of the fragments have a mass higher than predicted by the thermal Jeans mechanism, thus requiring external turbulence to explain it, and some of the fragments have a mass higher than 8 M which make them interesting targets for further studies. One of the fragment shows different molecular emissions tracing hot core, disk and outflows and is the most promising site for the search of high-mass stars toward RCW 120.

Published
2019

47. Fragmentation of massive cores toward the Galactic HII region RCW 120 observed with ALMA

Author

Figueira, Miguel, Bronfman, Leonardo, Zavagno, Annie, Louvet, Fabien, Lo, Nadia, Finger, Ricardo, Rodón, Javier, National Centre for Nuclear Research [Otwock], Narodowe Centrum Badań Jądrowych (NCBJ), 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 (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), Malek, Katarzyna and Polińska, Magdalena and Majczyna, Agnieszka and Stachowski, Grzegorz and Poleski, Rados\law and Wyrzykowski, Lukasz and Ró\.zańska, and Agata

Subjects
[SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; High-mass stars are primordial objects in the study of star formation since their feedback has a significant impact on the interstellar medium. The budget of momentum and energy of feedback can change the properties of the new generation of stars which is forming in the molecular cloud. \\\\We studied the galactic H II region RCW\raisebox-0.5ex~120 both in the far-infrared using the HERSCHEL space telescope and at millimetre wavelength using the ALMA interferometer. Almost all of the massive cores are found in the most massive clump and are fragmented differently. ALMA observations allowed us to characterize this fragmentation in order to see if these massive cores can give rise to high-mass stars. Most of the fragments have mass higher than the thermal Jeans mass, which can be explained by adding turbulence. A few fragments have a mass higher than 8\raisebox-0.5ex~M_ødot and could potentially be future sites of high-mass star formation. Molecular emissions in the most massive fragment of the most massive core indicate that the protostar is in the hot core phase.

Published
2019

48. VizieR Online Data Catalog: M16 CO maps (Xu+, 2019)

Author

Xu, J. -L., Zavagno, Annie, Yu, N., Liu, X. -L., Xu, Y., Yuan, J., Zhang, C. -P., Zhang, S. -J., Zhang, G. -Y., Ning, C. -C., Ju, B. -G., 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 de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), and Rice University [Houston]

Subjects
[SDU]Sciences of the Universe [physics], H II regions, Carbon monoxide
Abstract

CO data are observed by using the PMO 13.7m radio telescope. We map a 45'x45' region centered at l=17.023°, b=0.871° in the transitions of ^12CO J=1-0 (115.271GHz), ^13CO J=1-0 (110.201GHz), and C^18O J=1-0 (109.782GHz) lines. \\\\(2 data files).

Published
2019

49. VizieR Online Data Catalog: NGC 6357 massive dense cores (Russeil+, 2019)

Author

Russeil, D., Figueira, M., Zavagno, Annie, Motte, F., Schneider, N., Men'Shchikov, A., Bontemps, S., André, P., Anderson, L.~d., Benedettini, M., Didelon, P., Di, Francesco J., Elia, D., Koenyves, V., Nguyen Luong, Q., Nony, T., Pezzuto, S., Rygl, K.~l.~j., Schisano, E., Spinoglio, L., Tigé, J., White, G.~j., 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), Centro de Matemática e Aplicações Fundamentais (CMAF), Universidade de Lisboa = University of Lisbon (ULISBOA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], 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), FORMATION STELLAIRE 2020, 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), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), Korea Astronomy and Space Science Institute (KASI), NAOJ Chile Observatory, and National Astronomical Observatory of Japan (NAOJ)

Subjects
Interstellar medium, [SDU]Sciences of the Universe [physics], H II regions, Infrared sources
Abstract

International audience; Fluxes and information for the 23 massive dense cores (MDCs) found in NGC 6357. Information for 155 reliable sources. \\\\(4 data files).

Published
2019

50. VizieR Online Data Catalog: G345.5+1.5 region multiwavelength study (Figueira+, 2019)

Author

Figueira, M., Lopez-Calderon, C., Bronfman, L., Zavagno, Annie, Hervias-Caimapo, C., Duronea, N., Nyman, L. -A., and Beaussier, Catherine

Subjects
[SDU] Sciences of the Universe [physics], Radio lines, H II regions, Molecular clouds, Millimetric/submm sources
Abstract

Observation of the G345.5+1.5 region obtained with APEX-LABOCA at 870um and with NANTEN-2 for the ^12CO(4-3) transition line. \\\\Physical parameters of the clumps extracted from APEX LABOCA 870um (45 clumps, Clumpfind), Herschel Hi-GAL (79 clumps, CUTEX) and NANTEN2 ^12CO(4-3) (95 clumps, Clumpfind) \\\\(5 data files).

Published
2019

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