Author: "Cresci, G." / Topic: astrophysics - Searchworks@Jio Institute Digital Library Search Results

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84 results on '"Cresci, G."'

1. Mergers and Mass Accretion Rates in Galaxy Assembly: The Millennium Simulation Compared to Observations of z~2 Galaxies

Author: Genel, S., Genzel, R., Bouché, N., Sternberg, A., Naab, T., Schreiber, N. M. Förster, Shapiro, K. L., Tacconi, L. J., Lutz, D., Cresci, G., Buschkamp, P., Davies, R. I., and Hicks, E. K. S.
Subjects: Astrophysics
Abstract: Recent observations of UV-/optically selected, massive star forming galaxies at z~2 indicate that the baryonic mass assembly and star formation history is dominated by continuous rapid accretion of gas and internal secular evolution, rather than by major mergers. We use the Millennium Simulation to build new halo merger trees, and extract halo merger fractions and mass accretion rates. We find that even for halos not undergoing major mergers the mass accretion rates are plausibly sufficient to account for the high star formation rates observed in z~2 disks. On the other hand, the fraction of major mergers in the Millennium Simulation is sufficient to account for the number counts of submillimeter galaxies (SMGs), in support of observational evidence that these are major mergers. When following the fate of these two populations in the Millennium Simulation to z=0, we find that subsequent mergers are not frequent enough to convert all z~2 turbulent disks into elliptical galaxies at z=0. Similarly, mergers cannot transform the compact SMGs/red sequence galaxies at z~2 into observed massive cluster ellipticals at z=0. We argue therefore, that secular and internal evolution must play an important role in the evolution of a significant fraction of z~2 UV-/optically and submillimeter selected galaxy populations., Comment: 5 pages, 4 figures, Accepted for publication in ApJ
Published: 2008
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2. From rings to bulges: evidence for rapid secular galaxy evolution at z~2 from integral field spectroscopy in the SINS survey

Author: Genzel, R., Burkert, A., Bouche, N., Cresci, G., Schreiber, N. M. Foerster, Shapley, A., Shapiro, K., Tacconi, L. J., Buschkamp, P., Cimatti, A., Daddi, E., Davies, R., Eisenhauer, F., Erb, D. K., Genel, S., Gerhard, O., Hicks, E., Lutz, D., Naab, T., Ott, T., Rabien, S., Renzini, A., Steidel, C. C., Sternberg, A., and Lilly, S. J.
Subjects: Astrophysics
Abstract: We present Ha integral field spectroscopy of well resolved, UV/optically selected z~2 star-forming galaxies as part of the SINS survey with SINFONI on the ESO VLT. Our laser guide star adaptive optics and good seeing data show the presence of turbulent rotating star forming rings/disks, plus central bulge/inner disk components, whose mass fractions relative to total dynamical mass appears to scale with [NII]/Ha flux ratio and star formation age. We propose that the buildup of the central disks and bulges of massive galaxies at z~2 can be driven by the early secular evolution of gas-rich proto-disks. High redshift disks exhibit large random motions. This turbulence may in part be stirred up by the release of gravitational energy in the rapid cold accretion flows along the filaments of the cosmic web. As a result dynamical friction and viscous processes proceed on a time scale of <1 Gyr, at least an order of magnitude faster than in z~0 disk galaxies. Early secular evolution thus drives gas and stars into the central regions and can build up exponential disks and massive bulges, even without major mergers. Secular evolution along with increased efficiency of star formation at high surface densities may also help to account for the short time scales of the stellar buildup observed in massive galaxies at z~2., Comment: accepted Astrophysical Journal, main July 8 2008
Published: 2008
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3. Integral field near-infrared spectroscopy of II Zw 40

Author: Vanzi, L., Cresci, G., Telles, E., and Melnick, J.
Subjects: Astrophysics
Abstract: We present integral field spectroscopy in the near-infrared of the nearby starburst galaxy IIZw40. Our new observations provide an unprecedented detailed view of the interstellar medium and star formation of this galaxy. The radiation emitted by the galaxy is dominated by a giant HII region, which extends over an area of more than 400 pc in size. A few clusters are present in this area, however one in particular appears to be the main source of ionizing photons. We derive the properties of this object and compare them with those of the 30 Doradus cluster in the Large magellanic cloud (LMC). We study the spatial distribution and velocity field of different components of the inetrstellar medium (ISM), mostly through the Bracket series lines, the molecular hydrogen spectrum, and [FeII]. We find that [FeII] and H2 are mostly photon excited, but while the region emitting [FeII] is almost coincident with the giant HII region observed in the lines of atomic H and He, the H2 has a quite different distribution in space and velocity. The age of the stellar population in the main cluster is such that no supernova (SN) should be present yet so that the gas kinematics must be dominated by the young stars. We do not see, in the starbursting region, any geometrical or dynamical structure that can be related to the large scale morphology of the galaxy., Comment: Accepted for publication on A&A
Published: 2008
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4. Kinemetry of SINS High-Redshift Star-Forming Galaxies: Distinguishing Rotating Disks from Major Mergers

Author: Shapiro, K. L., Genzel, R., Schreiber, N. M. Forster, Tacconi, L. J., Bouche, N., Cresci, G., Davies, R., Eisenhauer, F., Johansson, P. H., Krajnovic, D., Lutz, D., Naab, T., Arimoto, N., Arribas, S., Cimatti, A., Colina, L., Daddi, E., Daigle, O., Erb, D., Hernandez, O., Kong, X., Mignoli, M., Onodera, M., Renzini, A., Shapley, A., and Steidel, C.
Subjects: Astrophysics
Abstract: We present a simple set of kinematic criteria that can distinguish between galaxies dominated by ordered rotational motion and those involved in major merger events. Our criteria are based on the dynamics of the warm ionized gas (as traced by H-alpha) within galaxies, making this analysis accessible to high-redshift systems, whose kinematics are primarily traceable through emission features. Using the method of kinemetry (developed by Krajnovic and co-workers), we quantify asymmetries in both the velocity and velocity dispersion maps of the warm gas, and the resulting criteria enable us to empirically differentiate between non-merging and merging systems at high redshift. We apply these criteria to 11 of our best-studied rest-frame UV/optical-selected z~2 galaxies for which we have near infrared integral field spectroscopic data from SINFONI on the VLT. Of these 11 systems, we find that >50% have kinematics consistent with a single rotating disk interpretation, while the remaining systems are more likely undergoing major mergers. This result, combined with the short formation timescales of these systems, provides evidence that rapid, smooth accretion of gas plays a significant role in galaxy formation at high redshift., Comment: Accepted for publication in the Astrophysical Journal. 24 pages, 14 figures
Published: 2008
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5. Dynamical Properties of z~2 Star Forming Galaxies and a Universal Star Formation Relation

Author: Bouche, N., Cresci, G., Davies, R., Eisenhauer, F., Schreiber, N. M. Forster, Genzel, R., Gillessen, S., Lehnert, M., Lutz, D., Nesvadba, N., Shapiro, K. L., Sternberg, A., Tacconi, L. J., Verma, A., Cimatti, A., Daddi, E., Renzini, A., Erb, D. K., Shapley, A., and Steidel, C. C.
Subjects: Astrophysics
Abstract: We present the first comparison of the dynamical properties of different samples of z~1.4-3.4 star forming galaxies from spatially resolved imaging spectroscopy from SINFONI/VLT integral field spectroscopy and IRAM CO millimeter interferometry. Our samples include 16 rest-frame UV-selected, 16 rest-frame optically-selected and 13 submillimeter galaxies (SMGs). We find that restframe UV- and optically bright (K<20) z~2 star forming galaxies are dynamically similar, and follow the same velocity-size relation as disk galaxies at z~0. In the theoretical framework of rotating disks forming from dissipative collapse in dark matter halos, the two samples require a spin parameter ranging from 0.06 to 0.2. In contrast bright SMGs have larger velocity widths and are much more compact. Hence, SMGs have lower angular momenta and higher matter densities than either of the UV- or optically selected populations. This indicates that dissipative major mergers may dominate the SMGs population, resulting in early spheroids, and that the majority of UV/optically bright galaxies have evolved less violently [...]. These early disks may later evolve into spheroids via disk instabilities or mergers. Because of their small sizes and large densities, SMGs lie at the high surface density end of a universal (out to z=2.5) "Schmidt-Kennicutt" relation between gas surface density and star formation rate surface density with a slope of ~1.7., Comment: 14 pages, 3 figures, accepted for publication in ApJ, minor typos corrected
Published: 2007
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6. A NICMOS search for obscured Supernovae in starburst galaxies

Author: Cresci, G., Mannucci, F., Della Valle, M., and Maiolino, R.
Subjects: Astrophysics
Abstract: The detection of obscured supernovae (SNe) in near-infrared monitoring campaigns of starburst galaxies has shown that a significant fraction of SNe is missed by optical surveys. However, the number of SNe detected in ground-based near-IR observations is still significantly lower than the number of SNe extrapolated from the FIR luminosity of the hosts. A possibility is that most SNe occur within the nuclear regions, where the limited angular resolution of ground-based observations prevents their detection. This issue prompted us to exploit the superior angular resolution of NICMOS-HST to search for obscured SNe within the first kpc from the nucleus of strong starbursting galaxies. A total of 17 galaxies were observed in SNAPSHOT mode. Based on their FIR luminosity, we expected to detect not less than ~12 SNe. However, no confirmed SN event was found. From our data we derive an observed nuclear SN rate <0.5 SN/yr per galaxy. The shortage of SN detections can be explained by a combination of several effects. The most important are: i) the existence of a strong extinction, A_V>11; ii) most SNe occur within the first 0.5" (which corresponds in our sample to about 500pc) where even NICMOS is unable to detect SN events., Comment: 7 pages, accepted for publication in A&A
Published: 2006
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7. Galaxy morphology and evolution from SWAN Adaptive Optics imaging

Author: Cresci, G., Davies, R. I., Baker, A. J., Mannucci, F., Lehnert, M. D., Totani, T., and Minowa, Y.
Subjects: Astrophysics
Abstract: We present the results from adaptive optics (AO) assisted imaging in the Ks band of an area of 15 arcmin^2 for SWAN (Survey of a Wide Area with NACO). We derive the high resolution near-IR morphology of ~400 galaxies up to Ks~23.5 in the first 21 SWAN fields around bright guide stars, carefully taking into account the survey selection effects and using an accurate treatment of the anisoplanatic AO PSF. The detected galaxies are sorted into two morphological classes according to their Sersic index. The extracted morphological properties and number counts of the galaxies are compared with the predictions of different galaxy formation and evolution models, both for the whole galaxy population and separately for late-type and early-type galaxies. This is one of the first times such a comparison has been done in the near-IR, as AO observations and accurate PSF modeling are needed to obtain reliable morphological classification of faint field galaxies at these wavelengths. For early-type galaxies we find that a pure luminosity evolution model, without evidence for relevant number and size evolution, better reproduces the observed properties of our Ks-selected sample than current semi-analytic models based on the hierarchical picture of galaxy formation. In particular, we find that the observed flattening of elliptical galaxy counts at Ks~20 is quantitatively in good agreement with the prediction of the pure luminosity evolution model that was calculated prior to the observation. For late-type galaxies, while both models are able to reproduce the number counts, we find some hints of a possible size growth. These results demonstrate the unique power of AO observations to derive high resolution details of faint galaxies' morphology in the near-IR and drive studies of galaxy evolution., Comment: 15 pages, 10 figures. A&A, in press. Final version with corrected typos
Published: 2006
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8. Accounting for anisoplanatic point spread function in deep wide-field adaptive optics images

Author: Cresci, G., Davies, R. I., Baker, A. J., and Lehnert, M. D.
Subjects: Astrophysics
Abstract: In this paper we present the approach we have used to determine and account for the anisoplanatic point spread function (PSF) in deep adaptive optics (AO) images for the Survey of a Wide Area with NACO (SWAN) at the ESO VLT. The survey comprises adaptive optics observations in the Ks band totaling ~ 30 arcmin^2, assembled from 42 discrete fields centered on different bright stars suitable for AO guiding. We develop a parametric model of the PSF variations across the field of view in order to build an accurate model PSF for every galaxy detected in each of the fields. We show that this approach is particularly convenient, as it uses only easily available data and makes no uncertain assumptions about the stability of the isoplanatic angle during any given night. The model was tested using simulated galaxy profiles to check its performance in terms of recovering the correct morphological parameters; we find that the results are reliable up to Ks ~ 20.5 (K_AB ~ 22.3) in a typical SWAN field. Finally, the model obtained was used to derive the first results from five SWAN fields, and to obtain the AO morphology of 55 galaxies brighter than Ks = 20. These preliminary results demonstrate the unique power of AO observations to derive the details of faint galaxy morphologies and to study galaxy evolution., Comment: 12 pages, 12 figures. Accepted for publication in A&A
Published: 2005
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9. The Star Cluster population of NGC 5253

Author: Cresci, G., Vanzi, L., and Sauvage, M.
Subjects: Astrophysics
Abstract: We present a detailed analysis of the star cluster population in the starburst galaxy NGC 5253. Our work is based on HST optical and VLT Ks images. We detect more than 300 clusters, and for all of them we derive the photometry in the V, I and Ks bands and built a color-color V-I/V-Ks diagram. After correction for star contamination, we matched 115 sources in all the three bands V, I and Ks. Comparison of the data points with models shows how most of the sources are affected by a red excess. The ages of the younger clusters are obtained from a HST Halpha image which allows to partially remove the degeneracy between age and extinction and to calculate the screen optical depth toward the clusters. The V and Ks luminosity functions show a marked turnover at M(V)=-7.3 and M(K)=-10.2, with a shape roughly similar to the gaussian distribution of old globular clusters. We convert the luminosity function into a mass function, and find that the clusters younger than 10 Myr show a power law distribution with slope -1.6, while the distribution of the older clusters has a maximum at about 4x10^4 Msun., Comment: 9 pages, 5 figures. Accepted for publication in A&A
Published: 2004
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10. The supernova rate per unit mass

Author: Mannucci, F., Della Valle, M., Panagia, N., Cappellaro, E., Cresci, G., Maiolino, R., Petrosian, A., and Turatto, M.
Subjects: Astrophysics
Abstract: We compute the rate of supernovae (SNe) of different types along the Hubble sequence normalized to the near-infrared luminosity and to the stellar mass of the parent galaxies. This is made possible by the new complete catalog of near-infrared galaxy magnitudes obtained by 2MASS. We find that the rates of all SN types, including Ia, Ib/c and II, show a sharp dependence on both the morphology and the (B-K) colors of the parent galaxies and, therefore, on the star formation activity. In particular we find, with a high statistical significance, that the type Ia rate in late type galaxies is a factor ~20 higher than in E/S0. Similarly, the type Ia rate in the galaxies bluer than B-K=2.6 is about a factor of 30 larger than in galaxies with B--K>4.1. These findings can be explained by assuming that a significant fraction of Ia events in late Spirals/Irregulars originates in a relatively young stellar component., Comment: 10 pages, A&A, in press
Published: 2004
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11. Nuclear star formation in the quasar PG1126-041 from adaptive optics assisted spectroscopy

Author: Cresci, G., Maiolino, R., Marconi, A., Mannucci, F., and Granato, G. L.
Subjects: Astrophysics
Abstract: We present adaptive optics assisted spectroscopy of three quasars obtained with NACO at VLT. The high angular resolution achieved with the adaptive optics (~0.08"), joined to the diagnostic power of near-IR spectroscopy, allow us to investigate the properties of the innermost 100 pc of these quasars. In the quasar with the best adaptive optics correction, PG1126-041, we spatially resolve the Pa-alpha emission within the nuclear 100 pc. The comparison with higher excitation lines suggests that the narrow Pa-alpha emission is due to nuclear star formation. The inferred intensity of the nuclear star formation (13 M(sun)/yr) may account for most of the far-IR luminosity observed in this quasar., Comment: 4 pages, 4 figures. Accepted for publication in A&A
Published: 2004
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12. The Infrared Supernova Rate

Author: Mannucci, F., Cresci, G., Maiolino, R., and Della Valle, M.
Subjects: Astrophysics
Abstract: Optical searches can only detect supernovae with a limited amount of dust extinction. This is a severe limitation as most of the core-collapse SNe could explode inside dusty regions. We describe a few ongoing projects aimed at detecting dusty SNe at near-IR wavelengths both in ground-based and HST images and to study their properties., Comment: 5 pages, IAU coll. 192 "Supernovae: 10 years of SN1993J", J.M. Marcaide and K.W. Weiler eds
Published: 2003

13. The infrared supernova rate in starburst galaxies

Author: Mannucci, F., Maiolino, R., Cresci, G., Della Valle, M., Vanzi, L., Ghinassi, F., Ivanov, V. D., Nagar, N. M., and Alonso-Herrero, A.
Subjects: Astrophysics
Abstract: We report the results of our ongoing search for extincted supernovae (SNe) at near-infrared wavelengths. We have monitored at 2.2 micron a sample of 46 Luminous Infrared Galaxies and detected 4 SNe. The number of detections is still small but sufficient to provide the first estimate of supernova rate at near-infrared wavelengths. We measure a SN rate ofv 7.6+/-3.8 SNu which is an order of magnitude larger than observed in quiescent galaxies. On the other hand, the observed near-infrared rate is still a factor 3-10 smaller than that estimated from the far-infrared luminosity of the galaxies. Among various possibilities, the most likely scenario is that dust extinction is so high (Av>30) to obscure most SNe even in the near-IR. The role of type Ia SNe is also discussed within this context. We derive the type Ia SN rate as a function of the stellar mass of the galaxy and find a sharp increase toward galaxies with higher activity of star formation. This suggests that a significant fraction of type Ia SNe are associated with young stellar populations. Finally, as a by-product, we give the average K-band light curve of core-collapse SNe based on all the existing data, and review the relation between SN rate and far-infrared luminosity., Comment: A&A, in press, 13 pages
Published: 2003
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14. Discovery of two infrared supernovae: a new window on the SN search

Author: Maiolino, R., Vanzi, L., Mannucci, F., Cresci, G., Ghinassi, F., and Della Valle, M.
Subjects: Astrophysics
Abstract: We report the discovery of two supernovae (SN 1999gw and SN 2001db) obtained within the framework of an infrared monitoring campaign of Luminous Infrared Galaxies, aimed at detecting obscured supernovae. SN 2001db, extinguished by Av~5.5 mag, is the first supernova discovered in the infrared which has received the spectroscopic confirmation. This result highlights the power of infrared monitoring in detecting obscured SNe and indicates that optical surveys are probably missing a significant fraction of SNe, especially in obscured systems such as starburst galaxies. The preliminary estimate of SN rate in LIRG galaxies is about an order of magnitude higher than that expected from optical surveys., Comment: 9 pages, 7 figures, accepted for publication in A&A
Published: 2002
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15. Dense and Warm Neutral Gas in BR 1202-0725 at z = 4.7 as Traced by the [O I] 145 μm Line

Author: Lee, MM, Nagao, T, De Breuck, C, Carniani, S, Cresci, G, Hatsukade, B, Kawabe, R, Kohno, K, Maiolino, R, Mannucci, F, Marconi, A, Nakanishi, K, Troncoso, P, Umehata, H, Lee, MM [0000-0002-2419-3068], Nagao, T [0000-0002-7402-5441], De Breuck, C [0000-0002-6637-3315], Carniani, S [0000-0002-6719-380X], Cresci, G [0000-0002-5281-1417], Hatsukade, B [0000-0001-6469-8725], Kawabe, R [0000-0002-8049-7525], Kohno, K [0000-0002-4052-2394], Maiolino, R [0000-0002-4985-3819], Mannucci, F [0000-0002-4803-2381], Marconi, A [0000-0002-9889-4238], Nakanishi, K [0000-0002-6939-0372], Troncoso, P [0000-0001-6162-3023], Umehata, H [0000-0003-1937-0573], Apollo - University of Cambridge Repository, Lee, M. M., Nagao, T., De Breuck, C., Carniani, S., Cresci, G., Hatsukade, B., Kawabe, R., Kohno, K., Maiolino, R., Mannucci, F., Marconi, A., Nakanishi, K., Troncoso, P., and Umehata, H.
Subjects: Quasars (1319), Physics, 010308 nuclear & particles physics, astro-ph.GA, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Submillimeter astronomy (1647), Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Interstellar line emission (844), Submillimetre astronomy, Settore FIS/05 - Astronomia e Astrofisica, Starburst galaxies (1570), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Galaxy evolution (594) [Unified Astronomy Thesaurus concepts], Line (formation)
Abstract: We report the detection of [O I]145.5um in the BR 1202-0725 system, a compact group at z=4.7 consisting of a quasar (QSO), a submillimeter-bright galaxy (SMG), and three faint Lya emitters. By taking into account the previous detections and upper limits, the [O I]/[C II] line ratios of the now five known high-z galaxies are higher than or on the high-end of the observed values in local galaxies ([O I]/[C II]$\gtrsim$0.13). The high [O I]/[C II] ratios and the joint analysis with the previous detection of [N II] lines for both the QSO and the SMG suggest the presence of warm and dense neutral gas in these highly star-forming galaxies. This is further supported by new CO (12-11) line detections and a comparison with cosmological simulations. There is a possible positive correlation between the [NII]122/205 line ratio and the [O I]/[C II] ratio when all local and high-z sources are taken into account, indicating that the denser the ionized gas, the denser and warmer the neutral gas (or vice versa). The detection of the [O I] line in the BR1202-0725 system with a relatively short amount of integration with ALMA demonstrates the great potential of this line as a dense gas tracer for high-z galaxies., STFC ERC
Published: 2021

16. A MUSE inquiry into the physical processes taking place within the Abell 2667 Brightest Cluster Galaxy

Author: Iani, E., Rodighiero, G., Fritz, J., Cresci, G., Mancini, C., Tozzi, P., Rodríguez-Muñoz, L., Rosati, P., Caminha, G. B., Berta, S., Cassata, P., Concas, A., Enia, A., Fadda, D., Franceschini, A., Liu, A., Mercurio, A., Morselli, L., Pérez-González, P. G., Popesso, P., Sabatini, G., Zanella, A., Boquien, M., Lusso, E., Gruppioni, C., Tissera, P., Iani, E., Rodighiero, G., Fritz, J., Cresci, G., Mancini, C., Tozzi, P., Rodríguez-Muñoz, L., Rosati, P., Caminha, G. B., Berta, S., Cassata, P., Concas, A., Enia, A., Fadda, D., Franceschini, A., Liu, A., Mercurio, A., Morselli, L., Pérez-González, P. G., Popesso, P., Sabatini, G., Zanella, A., and Astronomy
Subjects: 010504 meteorology & atmospheric sciences, Stellar mass, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, cD, (galaxies:) cooling flows, 0103 physical sciences, Cluster (physics), galaxies: elliptical and lenticular, Interacting galaxy, Brightest cluster galaxy, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Star formation, Astronomy and Astrophysics, Galaxy, Accretion (astrophysics), Universe, Space and Planetary Science, galaxies: elliptical and lenticular, cD, galaxies: kinematics and dynamic, galaxies: nuclei, galaxies: evolution
Abstract: Brightest cluster galaxies (BCGs) residing in cool-core clusters are known to be the stage of intricate baryon cycle phenomena (e.g. gas inflows, AGN outflows, star formation feedback). The scenarios describing the observed properties of these galaxies are still controversial, suffering from limitations due to the spatial resolving power of the instruments, specifically for galaxies beyond the Local Universe. However, the dramatic improvements introduced by the integral-field unit instruments (e.g. MUSE) could shed light on the physical processes driving the evolution of these galaxies. We present an extensive analysis of the stellar and gas properties (i.e. kinematics, stellar mass, star formation rate) of the radio-loud BCG sitting at the centre of the X-ray luminous cool-core cluster Abell 2667 (z = 0.23), based on MUSE data. Our results indicate that the BCG is a massive elliptical, hosting an AGN that is possibly undergoing accretion of cold star-forming clouds of ICM or galactic cannibalism.
Published: 2019

17. Evidence for Mature Bulges and an Inside-out Quenching Phase 3 Billion Years After the Big Bang

Author: Tacchella S., Carollo C. M., Renzini A., Förster Schreiber N. M., Lang P., Wuyts S., Cresci G., Dekel A., Genzel R., Lilly S. J., Mancini C., Newman S., Onodera M., Shapley A., Tacconi L., Woo J., and Zamorani G.
Subjects: Quenching, Physics, Solar mass, Multidisciplinary, Stellar mass, Star formation, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Billion years, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Stars, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Most present-day galaxies with stellar masses $\geq10^{11}$ solar masses show no ongoing star formation and are dense spheroids. Ten billion years ago, similarly massive galaxies were typically forming stars at rates of hundreds solar masses per year. It is debated how star formation ceased, on which timescales, and how this "quenching" relates to the emergence of dense spheroids. We measured stellar mass and star-formation rate surface density distributions in star-forming galaxies at redshift 2.2 with $\sim1$ kiloparsec resolution. We find that, in the most massive galaxies, star formation is quenched from the inside out, on timescales less than 1 billion years in the inner regions, up to a few billion years in the outer disks. These galaxies sustain high star-formation activity at large radii, while hosting fully grown and already quenched bulges in their cores., Comment: 12 (+23) pages, 4 (+10) figures, accepted version
Published: 2015
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18. The SINS/zC-SINF Survey of z~2 Galaxy Kinematics: Rest-frame Morphology, Structure, and Colors from Near-infrared Hubble Space Telescope Imaging

Author: Tacchella S., Lang P., Carollo C. M., Förster Schreiber N. M F, Renzini A., Shapley A. E., Wuyts S., Cresci G., Genzel R., Lilly S. J., Mancini C., Newman S. F., Tacconi L. J., Zamorani G., Davies R. I., Kurk J., and Pozzetti L.
Subjects: 010504 meteorology & atmospheric sciences, Stellar mass, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Bulge, 0103 physical sciences, kinematics and dynamics [galaxies], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Cosmic dust, Physics, Very Large Telescope, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), structure [galaxies], Astrophysics::Earth and Planetary Astrophysics, Sersic profile, high-redshift [galaxies]
Abstract: We present the analysis of HST $J$- and $H$-band imaging for 29 galaxies on the star-forming main sequence at $z\sim2$, which have Adaptive Optics VLT SINFONI integral field spectroscopy from our SINS/zC-SINF program. The SINFONI H$\alpha$ data resolve the on-going star-formation and the ionized gas kinematics on scales of $1-2$ kpc; the near-IR images trace the galaxies' rest-frame optical morphologies and distributions of stellar mass in old stellar populations at a similar resolution. The global light profiles of most galaxies show disk-like properties well described by a single S\'ersic profile with $n\sim1$, with only $\sim15%$ requiring a high $n>3$ S\'ersic index, all more massive than $10^{10}M_\odot$. In bulge+disk fits, about $40%$ of galaxies have a measurable bulge component in the light profiles, with $\sim15%$ showing a substantial bulge-to-total ratio $B/T\ge0.3$. This is a lower limit to the frequency of $z\sim2$ massive galaxies with a developed bulge component in stellar mass because it could be hidden by dust and/or outshined by a thick actively star-forming disk component. The galaxies' rest-optical half-light radii range between $1-7$ kpc, with a median of 2.1 kpc, and lie slightly above the size-mass relation at these epochs reported in the literature. This is attributed to differences in sample selection and definitions of size and/or mass measurements. The $(u-g)_{rest}$ color gradient and scatter within individual $z\sim2$ massive galaxies with $\ge10^{11}M_\odot$ are as high as in $z=0$ low-mass, late-type galaxies, and are consistent with the high star-formation rates of massive $z\sim2$ galaxies being sustained at large galactocentric distances., Comment: 25 pages (+11 pages appendix), 20 figures; accepted by ApJ
Published: 2014

19. LSD: Lyman-break galaxies Stellar populations and Dynamics – I. Mass, metallicity and gas at z∼ 3.1.

Author: Mannucci, F., Cresci, G., Maiolino, R., Marconi, A., Pastorini, G., Pozzetti, L., Gnerucci, A., Risaliti, G., Schneider, R., Lehnert, M., and Salvati, M.
Subjects: *GALAXY formation, *STAR formation, *NEAR infrared spectroscopy, *STELLAR mass, *REDSHIFT, *ASTROPHYSICS, *GAS dynamics
Abstract: We present the first results of a project, Lyman-break galaxies Stellar populations and Dynamics (LSD), aimed at obtaining spatially resolved, near-infrared (IR) spectroscopy of a complete sample of Lyman-break galaxies at . Deep observations with adaptive optics resulted in the detection of the main optical lines, such as [O ii]λ3727, Hβ and [O iii]λ5007, which are used to study sizes, star formation rates (SFRs), morphologies, gas-phase metallicities, gas fractions and effective yields. Optical, near-IR and Spitzer/Infrared Array Camera photometry are used to measure stellar mass. We obtain that morphologies are usually complex, with the presence of several peaks of emissions and companions that are not detected in broad-band images. Typical metallicities are 10–50 per cent solar, with a strong evolution of the mass–metallicity relation from lower redshifts. Stellar masses, gas fraction and evolutionary stages vary significantly among the galaxies, with less massive galaxies showing larger fractions of gas. In contrast with observations in the local universe, effective yields decrease with stellar mass and reach solar values at the low-mass end of the sample. This effect can be reproduced by gas infall with rates of the order of the SFRs. Outflows are present but are not needed to explain the mass–metallicity relation. We conclude that a large fraction of these galaxies is actively creating stars after major episodes of gas infall or merging. [ABSTRACT FROM AUTHOR]
Published: 2009
Full Text: View/download PDF

20. Euclid Definition Study Report

Author: Laureijs, R., Amiaux, J., Arduini, S., Augueres, J. L., Brinchmann, J., Cole, R., Cropper, M., Dabin, C., Duvet, L., Ealet, A., Garilli, B., Gondoin, P., Guzzo, L., Hoar, J., Hoekstra, H., Holmes, R., Kitching, T., Maciaszek, T., Mellier, Y., Pasian, F., Percival, W., Rhodes, J., Criado, G. Saavedra, Sauvage, M., Scaramella, R., Valenziano, L., Warren, S., Bender, R., Castander, F., Cimatti, A., Le, O., Kurki-Suonio, H., Levi, M., Lilje, P., Meylan, G., Nichol, R., Pedersen, K., Popa, V., Rebolo Lopez, R., Rix, H. W., Rottgering, H., Zeilinger, W., Grupp, F., Hudelot, P., Massey, R., Meneghetti, M., Miller, L., Paltani, S., Paulin-Henriksson, S., Pires, S., Saxton, C., Schrabback, T., Seidel, G., Walsh, J., Aghanim, N., Amendola, L., Bartlett, J., Baccigalupi, C., Beaulieu, J. P., Benabed, K., Cuby, J. G., Elbaz, D., Fosalba, P., Gavazzi, G., Helmi, A., Hook, I., Irwin, M., Kneib, J. P., Kunz, M., Mannucci, F., Moscardini, L., Tao, C., Teyssier, R., Weller, J., Zamorani, G., Osorio, M. R. Zapatero, Boulade, O., Foumond, J. J., Di Giorgio, A., Guttridge, P., James, A., Kemp, M., Martignac, J., Spencer, A., Walton, D., Blumchen, T., Bonoli, C., Bortoletto, F., Cerna, C., Corcione, L., Fabron, C., Jahnke, K., Ligori, S., Madrid, F., Martin, L., Morgante, G., Pamplona, T., Prieto, E., Riva, M., Toledo, R., Trifoglio, M., Zerbi, F., Abdalla, F., Douspis, M., Grenet, C., Borgani, S., Bouwens, R., Courbin, F., Delouis, J. M., Dubath, P., Fontana, A., Frailis, M., Grazian, A., Koppenhofer, J., Mansutti, O., Melchior, M., Mignoli, M., Mohr, J., Neissner, C., Noddle, K., Poncet, M., Scodeggio, M., Serrano, S., Shane, N., Starck, J. L., Surace, C., Taylor, A., Verdoes-Kleijn, G., Vuerli, C., Williams, O. R., Zacchei, A., Altieri, B., Sanz, I. Escudero, Kohley, R., Oosterbroek, T., Astier, P., Bacon, D., Bardelli, S., Baugh, C., Bellagamba, F., Benoist, C., Bianchi, D., Biviano, A., Branchini, E., Carbone, C., Cardone, V., Clements, D., Colombi, S., Conselice, C., Cresci, G., Deacon, N., Dunlop, J., Fedeli, C., Fontanot, F., Franzetti, P., Giocoli, C., Juan Garcia-Bellido, Gow, J., Heavens, A., Hewett, P., Heymans, C., Holland, A., Huang, Z., Ilbert, O., Joachimi, B., Jennins, E., Kerins, E., Kiessling, A., Kirk, D., Kotak, R., Krause, O., Lahav, O., Leeuwen, F., Lesgourgues, J., Lombardi, M., Magliocchetti, M., Maguire, K., Majerotto, E., Maoli, R., Marulli, F., Maurogordato, S., Mccracken, H., Mclure, R., Melchiorri, A., Merson, A., Moresco, M., Nonino, M., Norberg, P., Peacock, J., Pello, R., Penny, M., Pettorino, V., Di Porto, C., Pozzetti, L., Quercellini, C., Radovich, M., Rassat, A., Roche, N., Ronayette, S., Rossetti, E., Sartoris, B., Schneider, P., Semboloni, E., Serjeant, S., Simpson, F., Skordis, C., Smadja, G., Smartt, S., Spano, P., Spiro, S., Sullivan, M., Tilquin, A., Trotta, R., Verde, L., Wang, Y., Williger, G., Zhao, G., Zoubian, J., Zucca, E., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'Astrophysique de Marseille (LAM), 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), XMM-Newton Science Operations Centre, European Space Agency (ESA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AIR:SURFACES+DBI, Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), CNR Institute of Atmospheric Sciences and Climate (ISAC), Consiglio Nazionale delle Ricerche (CNR), Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), AUTRES, Institut Bisontin en Sciences Fondamentales (IBSF), Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, LAME, Laboratoire de Spectrométrie Physique (LSP), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Earth and Biosphere Institute, School of Geography, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Università degli studi di Trieste, Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Departament d'Astronomia i Meteorologia [Barcelona], Universitat de Barcelona (UB), Department of Physics [Hong Kong University of Science and Technology], Hong Kong University of Science and Technology (HKUST), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Centre National d'Études Spatiales [Toulouse] (CNES), Geneva Observatory, University of Geneva [Switzerland], Department of Surgical Oncology, University of Groningen [Groningen], Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique, Centre de recherches Paul Pascal (CRPP), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institute of Space Science [Bucharest-Măgurele] (ISS), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], ISDC Data Centre for Astrophysics, Department of Astronomy, Stanford University, Istituto Nazionale di Fisica Nucleare [Pisa] (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Departament Llenguatges i Sistemes Informatics, Universitat Politècnica de Catalunya [Barcelona] (UPC), University of Oxford Astrophysics, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), INAF - Osservatorio Astrofisico di Torino (OATo), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), Dipartimento di Ingegneria Idraulica, Ambientale, Infrastrutture Viarie, Rilevamento, ICT Institute of Politecnico di Milano, UCO/Lick Observatory, University of California [Santa Cruz] (UCSC), University of California-University of California, ISDC (ISDC), Dipartimento di Fisica [Povo], Università degli Studi di Trento (UNITN), INAF - Osservatorio Astronomico di Roma (OAR), foreign laboratories (FL), CERN [Genève], Forschungszentrum Karlsruhe (FZK), INAF- Milano, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Università degli Studi di Roma 'La Sapienza' [Rome], Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut de Ciènces del Cosmos (ICC), Universitat de Barcelona (UB)-Universitat de Barcelona (UB), Department of Physics [Kowloon], Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Brera (INAF), Universidade do Porto [Porto], Università di Bologna [Bologna] (UNIBO), Stanford University [Stanford], National Institute for Nuclear Physics (INFN), Universitá degli Studi di Milano-Bicocca, Universitá degli Studi di Milan-Bocca, Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico (OAR), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Cosmology and Extragalactic Astrophysics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Galaxy Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics of Galaxies (astro-ph.GA), [INFO]Computer Science [cs], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Galaxy Astrophysics
Abstract: Euclid is a space-based survey mission from the European Space Agency designed to understand the origin of the Universe's accelerating expansion. It will use cosmological probes to investigate the nature of dark energy, dark matter and gravity by tracking their observational signatures on the geometry of the universe and on the cosmic history of structure formation. The mission is optimised for two independent primary cosmological probes: Weak gravitational Lensing (WL) and Baryonic Acoustic Oscillations (BAO). The Euclid payload consists of a 1.2 m Korsch telescope designed to provide a large field of view. It carries two instruments with a common field-of-view of ~0.54 deg2: the visual imager (VIS) and the near infrared instrument (NISP) which contains a slitless spectrometer and a three bands photometer. The Euclid wide survey will cover 15,000 deg2 of the extragalactic sky and is complemented by two 20 deg2 deep fields. For WL, Euclid measures the shapes of 30-40 resolved galaxies per arcmin2 in one broad visible R+I+Z band (550-920 nm). The photometric redshifts for these galaxies reach a precision of dz/(1+z) < 0.05. They are derived from three additional Euclid NIR bands (Y, J, H in the range 0.92-2.0 micron), complemented by ground based photometry in visible bands derived from public data or through engaged collaborations. The BAO are determined from a spectroscopic survey with a redshift accuracy dz/(1+z) =0.001. The slitless spectrometer, with spectral resolution ~250, predominantly detects Ha emission line galaxies. Euclid is a Medium Class mission of the ESA Cosmic Vision 2015-2025 programme, with a foreseen launch date in 2019. This report (also known as the Euclid Red Book) describes the outcome of the Phase A study., 116 pages, with executive summary and table of contents

21. SUPER. V. ALMA continuum observations of z ∼ 2 AGN and the elusive evidence of outflows influencing star formation

Author: C. Cicone, Alessandro Marconi, Annagrazia Puglisi, Jakub Scholtz, Chiara Feruglio, M. Bischetti, Fabrizio Fiore, Enrico Piconcelli, Cristian Vignali, G. Vietri, M. Schramm, Isabella Lamperti, David J. Rosario, D. Kakkad, Stefano Carniani, V. Mainieri, C. Circosta, Luca Zappacosta, G. Calistro Rivera, Giovanni Cresci, David M. Alexander, L. N. Martínez-Ramírez, Christopher Harrison, Hagai Netzer, Michele Perna, Chian-Chou Chen, Filippo Mannucci, Lamperti I., Harrison C.M., Mainieri V., Kakkad D., Perna M., Circosta C., Scholtz J., Carniani S., Cicone C., Alexander D.M., Bischetti M., Calistro Rivera G., Chen C.-C., Cresci G., Feruglio C., Fiore F., Mannucci F., Marconi A., Martinez-Ramirez L.N., Netzer H., Piconcelli E., Puglisi A., Rosario D.J., Schramm M., Vietri G., Vignali C., Zappacosta L., Lamperti, I., Harrison, C. M., Mainieri, V., Kakkad, D., Perna, M., Circosta, C., Scholtz, J., Carniani, S., Cicone, Claudia, Alexander, D. M., Bischetti, Manuela, Calistro Rivera, G., Chen, C. -C., Cresci, Giovanni, Feruglio, Chiara, Fiore, Fabrizio, Mannucci, Filippo, Marconi, Alessandro, Martínez-Ramírez, L. N., Netzer, H., Piconcelli, Enrico, Puglisi, Alfio Timothy, Rosario, D. J., Schramm, M., Vietri, Giustina, Vignali, C., Zappacosta, Luca, DEU, Cicone, C., Bischetti, M., Cresci, G., Feruglio, C., Fiore, F., Mannucci, F., Marconi, A., Martinez-Ramirez, L. N., Piconcelli, E., Puglisi, A., Vietri, G., and Zappacosta, L.
Subjects: Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Seyfert [galaxies], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, ISM [galaxies], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: Seyfert, Stars, Photometry (astronomy), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, active [galaxies], Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], galaxies: ISM
Abstract: We study the impact of AGN ionised outflows on star formation in high-redshift AGN hosts, by combining NIR IFS observations, mapping the H$\alpha$ emission and [OIII] outflows, with matched-resolution observations of the rest-frame FIR emission. We present high-resolution ALMA Band 7 observations of eight X-ray selected AGN at z~2 from the SUPER sample, targeting the rest-frame ~260 um continuum at ~2 kpc (0.2'') resolution. We detected 6 out of 8 targets with S/N>10 in the ALMA maps, with continuum flux densities F = 0.27-2.58 mJy and FIR half-light radii Re = 0.8-2.1 kpc. The FIR Re of our sample are comparable to other AGN and star-forming galaxies at a similar redshift from the literature. However, we find that the mean FIR size in X-ray AGN (Re = 1.16+/- 0.11 kpc) is slightly smaller than in non-AGN (Re = 1.69+/-0.13 kpc). From SED fitting, we find that the main contribution to the 260 um flux density is dust heated by star formation, with < 4% contribution from AGN-heated dust and < 1% from synchrotron emission. The majority of our sample show different morphologies for the FIR (mostly due to reprocessed stellar emission) and the ionised gas emission (H$\alpha$ and [OIII], mostly due to AGN emission). This could be due to the different locations of dust and ionised gas, the different sources of the emission (stars and AGN), or the effect of dust obscuration. We are unable to identify any residual H$\alpha$ emission, above that dominated by AGN, that could be attributed to star formation. Under the assumption that the FIR emission is a reliable tracer of obscured star formation, we find that the obscured star formation activity in these AGN host galaxies is not clearly affected by the ionised outflows. However, we cannot rule out that star formation suppression is happening on smaller spatial scales than the ones we probe with our observations (< 2 kpc) or on different timescales., Comment: 32 pages, 13 figures. Accepted for publication in A&A
Published: 2021

22. Galaxy-scale ionised winds driven by ultra-fast outflows in two nearby quasars

Author: Emanuele Nardini, A. Marasco, S. di Serego Alighieri, Filippo Mannucci, Marcella Brusa, Stefano Carniani, A. Amiri, Paolo Tozzi, Enrico Piconcelli, Alessandro Marconi, G. Tozzi, Giacomo Venturi, Michele Perna, Giorgio Lanzuisi, Giovanni Cresci, Matilde Mingozzi, Francesco Tombesi, Marasco, A. [0000-0002-5655-6054], Cresci, G. [0000-0002-5281-1417], Nardini, E. [0000-0001-9226-8992], Manucci, F. [0000-0002-4803-2381], Marconi, A. [0000-0002-9889-4238], Tozzi, G. [0000-0003-4226-7777], Amiri, A. [0000-0002-8553-1964], Venturi, G. [0000-0001-8349-3055], Piconcelli, E. [0000-0001-9095-2782], Lanzuisi, G. [0000-0001-9094-0984], Tombesi, F. [0000-0002-6562-8654], Mingozzi, M. [0000-0003-2589-762X], Perna, M. [0000-0002-0362-5941], Carniani, S. [0000-0002-6719-380X], Brusa, M. [0000-0002-5059-6848], Di Serego Alighieri, S. [0000-0001-8769-2692], Istituto Nazionale Astrofisica (INAF), Marasco, A., Cresci, G., Nardini, E., Mannucci, F., Marconi, A., Tozzi, P., Tozzi, G., Amiri, A., Venturi, G., Piconcelli, E., Lanzuisi, G., Tombesi, F., Mingozzi, M., Perna, M., Carniani, S., Brusa, M., DI Serego Alighieri, S., Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, and Agenzia Spaziale Italiana (ASI)
Subjects: QSOS, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Kinetic energy, 01 natural sciences, PG 1126−041, 0103 physical sciences, ISM [Galaxies], quasars: individual: MR2251178 – quasars: individual: PG 1126041 – ISM: jets and outflows – techniques: imaging spectroscopy – galaxies: ISM, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ISM, Astrophysics::Galaxy Astrophysics, quasars: individual: MR 2251-178, quasars: individual: PG 1126-041, ISM: jets and outflows, techniques: imaging spectroscopy, galaxies: ISM, Line (formation), Physics, Settore FIS/05, 010308 nuclear & particles physics, imaging spectroscopy [Techniques], individual [Quasars], Velocity dispersion, Astronomy and Astrophysics, Quasar, MR 2251-178, jets and outflows, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow
Abstract: We used MUSE adaptive optics data in narrow field mode to study the properties of the ionised gas in MR 2251-178 and PG 1126-041, two nearby (z0.06) bright quasars (QSOs) hosting sub-pc scale ultra-fast outflows (UFOs) detected in the X-ray band. We decomposed the optical emission from diffuse gas into a low- and a high-velocity components. The former is characterised by a clean, regular velocity field and a low (∼80 km s-1) velocity dispersion. It traces regularly rotating gas in PG 1126-041, while in MR 2251-178 it is possibly associated with tidal debris from a recent merger or flyby. The other component is found to be extended up to a few kpc from the nuclei, and shows a high (∼800 km s-1) velocity dispersion and a blue-shifted mean velocity, as is expected from outflows driven by active galactic nuclei (AGN). We estimate mass outflow rates up to a few Mpdbl yr-1 and kinetic efficiencies LKIN/LBOL between 1-4 × 10-4, in line with those of galaxies hosting AGN of similar luminosities. The momentum rates of these ionised outflows are comparable to those measured for the UFOs at sub-pc scales, which is consistent with a momentum-driven wind propagation. Pure energy-driven winds are excluded unless about 100× additional momentum is locked in massive molecular winds. In comparing the outflow properties of our sources with those of a small sample of well-studied QSOs hosting UFOs from the literature, we find that winds seem to systematically lie either in a momentum-driven or an energy-driven regime, indicating that these two theoretical models bracket the physics of AGN-driven winds very well., Marasco, A.; Cresci, G.; Nardini, E.; Mannucci, F.; Marconi, A.; Tozzi, P.; Tozzi, G.; Amiri, A.; Venturi, G.; Piconcelli, E.; Lanzuisi, G.; Tombesi, F.; Mingozzi, M.; Perna, M.; Carniani, S.; Brusa, M.; DI Serego Alighieri, S.
Published: 2020

23. The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies

Author: A. Pensabene, Stefano Carniani, Roberto Decarli, Roberto Maiolino, Alessandro Marconi, Michele Perna, Giovanni Cresci, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Pensabene, A. [0000-0001-9815-4953], Carniani, S. [0000-0002-6719-380X], Perna, M. [0000-0002-0362-5941], Cresci, G. [0000-0002-5281-1417], Decarli, R. [0000-0002-2662-8803], Marconi, A. [0000-0002-9889-4238], European Research Council (ERC), Comunidad de Madrid, Pensabene, A., Carniani, S., Perna, M., Cresci, G., Decarli, R., Maiolino, R., Marconi, A., Comunidad de Madrid, Programa Atracción de Talento 2018-T2/TIC-11715, Pensabene A., Carniani S., Perna M., Cresci G., Decarli R., Maiolino R., and Marconi A.
Subjects: Active galactic nucleus, media_common.quotation_subject, Quasars: supermassive black holes, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, high-redshift [Galaxies], Galaxies: kinematics and dynamic, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Galaxy formation and evolution, supermassive black hole [Quasars], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Supermassive black hole, kinematics and dynamic [Galaxies], 010308 nuclear & particles physics, Star formation, kinematics and dynamics [Galaxies], Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Quasar, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Universe, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), high redshift [Galaxies], supermassive black holes [Quasars]
Abstract: Context. The existence of tight correlations between supermassive black holes (BHs) and their host galaxies' properties in the local Universe suggests a closely linked evolution. Investigating these relations up to the high redshifts (z ≳ 6) is crucial in order to understand the interplay between star formation and BH growth across the cosmic time and to set constraints on galaxy formation and evolution models. In this work, we focus on the relation between BH mass (MBH) and the dynamical mass (Mdyn) of the host galaxy. Aims. Previous works suggest an evolution of the MBH-Mdyn relation with redshift indicating that BH growth precedes the galaxy mass assembly during their co-evolution at z > 3. However, dynamical galaxy masses at high redshift are often estimated through the virial theorem, thus introducing significant uncertainties. Within the scope of this work, our aim is to study the MBH-Mdyn relation of a sample of 2 < z < 7 quasars by constraining their galaxy masses through a full kinematical modelling of the cold gas kinematics, thus avoiding all possible biases and effects introduced by the rough estimates usually adopted so far. Methods. For this purpose, we retrieved public observations of 72 quasar host galaxies observed in [CII]158 μm or CO transitions with the Atacama Large Millimeter Array (ALMA). We then selected those quasars whose line emission is spatially resolved, and performed a kinematic analysis on ALMA observations. We estimated the dynamical mass of the systems by modelling the gas kinematics with a rotating disc, taking into account geometrical and instrumental effects. Our dynamical mass estimates, combined with MBH obtained from literature and our own new CIVλ1550 observations allowed us to investigate the MBH/Mdyn in the early Universe. Results. Overall, we obtained a sample of ten quasars at z ∼ 2-7, in which line emission is detected with high S/N (≳ 5-10) and the gas kinematics are spatially resolved and dominated by ordered rotation. The estimated dynamical masses place six out of ten quasars above the local relation yielding to MBH/Mdyn ratios ∼10× higher than those estimated in low-z galaxies. On the other hand, we found that four quasars at z ∼ 4-6 have dynamical-to-BH-mass ratios consistent with what is observed in early-type galaxies in the local Universe., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
Published: 2020

24. SUPER: III. Broad line region properties of AGNs at z ∼ 2

Author: Michele Perna, Giorgio Lanzuisi, G. Vietri, Andrea Comastri, Angela Bongiorno, S. Carniani, Marcella Brusa, M. Bischetti, Alessandro Marconi, Hagai Netzer, C. Circosta, Chiara Feruglio, Giovanni Cresci, Jakub Scholtz, Christopher Harrison, Annagrazia Puglisi, Fabrizio Fiore, Enrico Piconcelli, F. Mannucci, Andreas Schulze, Mara Salvato, G. Zamorani, D. Kakkad, Luca Zappacosta, Paolo Padovani, C. Cicone, Bernd Husemann, M. Schramm, Cristian Vignali, Vincenzo Mainieri, Vietri, Giustina, Mainieri, V., Kakkad, D., Netzer, H., Perna, M., Circosta, C., Harrison, C. M., Zappacosta, Luca, Husemann, B., Padovani, P., Bischetti, Manuela, Bongiorno, Angela, Brusa, M., Carniani, S., Cicone, Claudia, Comastri, Andrea, Cresci, Giovanni, Feruglio, Chiara, Fiore, Fabrizio, Lanzuisi, Giorgio, Mannucci, Filippo, Marconi, Alessandro, Piconcelli, Enrico, Puglisi, Alfio Timothy, Salvato, M., Schramm, M., Schulze, A., Scholtz, J., Vignali, C., Zamorani, G., Vietri, G., Zappacosta, L., Bischetti, M., Bongiorno, A., Cicone, C., Comastri, A., Cresci, G., Feruglio, C., Fiore, F., Lanzuisi, G., Mannucci, F., Marconi, A., Piconcelli, E., Puglisi, A., Vietri G., Mainieri V., Kakkad D., Netzer H., Perna M., Circosta C., Harrison C.M., Zappacosta L., Husemann B., Padovani P., Bischetti M., Bongiorno A., Brusa M., Carniani S., Cicone C., Comastri A., Cresci G., Feruglio C., Fiore F., Lanzuisi G., Mannucci F., Marconi A., Piconcelli E., Puglisi A., Salvato M., Schramm M., Schulze A., Scholtz J., Vignali C., and Zamorani G.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, supermassive black holes [quasars], Quasars: emission line, quasars: supermassive black holes, Balmer series, Astronomy and Astrophysics, Redshift, Galaxy, Blueshift, emission line [quasars], Black hole, quasars: emission lines, Space and Planetary Science, galaxies: evolution, active [galaxies], symbols, H-alpha, Equivalent width, high-redshift [galaxies]
Abstract: Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) was designed to conduct a blind search for AGN-driven outflows on X-ray-selected AGNs at redshift z∼2 with high (∼2 kpc) spatial resolution, and to correlate them with the properties of their host galaxy and central black hole. The main aims of this paper are: (a) to derive reliable estimates for the masses of the black holes and accretion rates for the Type-1 AGNs in this survey; and (b) to characterise the properties of the AGN-driven winds in the broad line region (BLR). Methods. We analysed rest-frame optical and UV spectra of 21 Type-1 AGNs. We used Hα, Hβ, and MgII line profiles to estimate the masses of the black holes. We used the blueshift of the CIV line profile to trace the presence of winds in the BLR. Results. We find that the Hα and Hβ line widths are strongly correlated, as is the line continuum luminosity at 5100 Å with Hα line luminosity, resulting in a well-defined correlation between black hole masses estimated from Hα and Hβ. Using these lines, we estimate that the black hole masses for our objects are in the range Log (MBH/M·) = 8.4-10.8 and are accreting at λEdd = 0.04-1.3. Furthermore, we confirm the well-known finding that the CIV line width does not correlate with the Balmer lines and the peak of the line profile is blueshifted with respect to the [OIII]-based systemic redshift. These findings support the idea that the CIV line is tracing outflowing gas in the BLR for which we estimated velocities up to ∼4700 km s-1. We confirm the strong dependence of the BLR wind velocity on the UV-to-X-ray continuum slope, the bolometric luminosity, and Eddington ratio. We infer BLR mass outflow rates in the range 0.005-3 M· yr-1, revealing a correlation with the bolometric luminosity consistent with that observed for ionised winds in the narrow line region (NLR), and X-ray winds detected in local AGNs, and kinetic power ∼10-7-10-4 × LBol. The coupling efficiencies predicted by AGN-feedback models are much higher than the values reported for the BLR winds in the SUPER sample; although it should be noted that only a fraction of the energy injected by the AGN into the surrounding medium is expected to become kinetic power in the outflow. Finally, we find an anti-correlation between the equivalent width of the [OIII] line and the CIV velocity shift, and a positive correlation between this latter parameter and [OIII] outflow velocity. These findings, for the first time in an unbiased sample of AGNs at z∼2, support a scenario where BLR winds are connected to galaxy-scale detected outflows, and are therefore capable of affecting the gas in the NLR located at kiloparsec scale distances., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
Published: 2020

25. SUPER IV. CO(J=3-2) properties of active galactic nucleus hosts at cosmic noon revealed by ALMA

Author: Christopher Harrison, Chiara Feruglio, G. Vietri, Bernd Husemann, Alessandro Marconi, Filippo Mannucci, Luca Zappacosta, Stefano Carniani, Annagrazia Puglisi, Giorgio Lanzuisi, Giovanni Cresci, C. Circosta, M. Schramm, Mara Salvato, D. Kakkad, A. Zanella, Marcella Brusa, C. Cicone, Amélie Saintonge, Isabella Lamperti, M. Bischetti, Enrico Piconcelli, Cristian Vignali, Michele Perna, Paolo Padovani, V. Mainieri, Circosta, C., Mainieri, V., Lamperti, I., Padovani, P., Bischetti, M., Harrison, C. M., Kakkad, D., Zanella, Anita, Vietri, G., Lanzuisi, G., Salvato, M., Brusa, M., Carniani, Stefano, Cicone, Claudia, Cresci, G., Feruglio, Chiara, Husemann, B., Mannucci, Filippo, Marconi, Alessandro, Perna, Marianna, Piconcelli, Enrico, Puglisi, Alessandra, Saintonge, A., Schramm, M., Vignali, C., Zappacosta, L., Mannucci, F. [0000-0002-4803-2381], Science and Technology Facilities Council (STFC), Comunidad de Madrid, Bischetti, Manuela, Zanella, A., Vietri, Giustina, Lanzuisi, Giorgio, Carniani, S., Cresci, Giovanni, Perna, M., Puglisi, Alfio Timothy, Zappacosta, Luca, Circosta C., Mainieri V., Lamperti I., Padovani P., Bischetti M., Harrison C.M., Kakkad D., Zanella A., Vietri G., Lanzuisi G., Salvato M., Brusa M., Carniani S., Cicone C., Cresci G., Feruglio C., Husemann B., Mannucci F., Marconi A., Perna M., Piconcelli E., Puglisi A., Saintonge A., Schramm M., Vignali C., and Zappacosta L.
Subjects: Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, active–galaxies:evolution–galaxies:ISM–quasars:general–submillimeter:ISM–galaxies:high-redshift [galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, high-redshift [Galaxies], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, ISM [Galaxies], Submillimeter: ISM, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, ISM [Submillimeter], Galaxies: evolution, Astronomy and Astrophysics, general [Quasars], Galaxies: active, evolution [Galaxies], galaxies:active–galaxies:evolution–galaxies:ISM–quasars:general–submillimeter:ISM–galaxies:high-redshift, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Quasars: general, Galaxies: ISM, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), high redshift [Galaxies], Order of magnitude
Abstract: Feedback from AGN is thought to be key in shaping the life cycle of their host galaxies by regulating star-formation activity. Therefore, to understand the impact of AGN on star formation, it is essential to trace the molecular gas out of which stars form. In this paper we present the first systematic study of the CO properties of AGN hosts at z~2 for a sample of 27 X-ray selected AGN spanning two orders of magnitude in AGN bolometric luminosity (Lbol= 10^44.7-10^46.9 erg/s) by using ALMA Band 3 observations of the CO(3-2) transition (~1" angular resolution). To search for evidence of AGN feedback on the CO properties of the host galaxies, we compared our AGN with a sample of inactive (i.e., non-AGN) galaxies from the PHIBSS survey with similar redshift, stellar masses, and SFRs. We used the same CO transition as a consistent proxy for the gas mass for the two samples in order to avoid systematics involved when assuming conversion factors. By adopting a Bayesian approach to take upper limits into account, we analyzed CO luminosities as a function of stellar masses and SFRs, as well as the ratio LCO(3-2)/M* (proxy for the gas fraction). The two samples show statistically consistent trends in the LCO(3-2)-Lfir and LCO(3-2)-M* planes. However, there are indications that AGN feature lower CO(3-2) luminosities (0.4-0.7 dex) than inactive galaxies at the 2-3sigma level when we focus on the subset of parameters where the results are better constrained and on the distribution of the mean LCO(3-2)/M*. Therefore, even by conservatively assuming the same excitation factor r31, we would find lower molecular gas masses in AGN, and assuming higher r31 would exacerbate this difference. We interpret our result as a hint of the potential effect of AGN activity (e.g., radiation and outflows), which may be able to heat, excite, dissociate, and/or deplete the gas reservoir of the host galaxies. (abridged), Comment: Key figures: 2, 3, 4. 22 pages, 9 figures (5 in appendices), 3 tables. Accepted for publication in A&A
Published: 2020
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26. The gentle monster PDS 456: Kiloparsec-scale molecular outflow and its implications for QSO feedback

Author: Marcella Brusa, M. Bischetti, Chiara Feruglio, Fabrizio Fiore, Luca Zappacosta, C. Vignali, Enrico Piconcelli, Giovanni Cresci, Alessandro Marconi, Emanuele Nardini, Vincenzo Mainieri, Angela Bongiorno, S. Carniani, Claudia Cicone, Roberto Maiolino, Maiolino, Roberto [0000-0002-4985-3819], Apollo - University of Cambridge Repository, Bischetti, Manuela, Piconcelli, Enrico, Feruglio, Chiara, Fiore, Fabrizio, Carniani, S., Brusa, M., Cicone, Claudia, Vignali, C., Bongiorno, Angela, Cresci, Giovanni, Mainieri, V., Maiolino, R., Marconi, Alessandro, Nardini, Emanuele, Zappacosta, Luca, Bischetti M., Piconcelli E., Feruglio C., Fiore F., Carniani S., Brusa M., Cicone C., Vignali C., Bongiorno A., Cresci G., Mainieri V., Maiolino R., Marconi A., Nardini E., Zappacosta L., ITA, GBR, DEU, Bischetti, M., Piconcelli, E., Feruglio, C., Fiore, F., Cicone, C., Bongiorno, A., Cresci, G., Marconi, A., Nardini, E., and Zappacosta, L.
Subjects: quasars individual PDS456, quasars emission lines, quasars: individual: PDS 456, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), galaxies: active, galaxies active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, galaxies: active, quasars: individual: PDS 456, galaxies: evolution, quasars: emission lines, techniques: imaging spectroscopy, techniques: interferometric, Astrophysics - Astrophysics of Galaxies, 010308 nuclear & particles physics, imaging spectroscopy [Techniques], techniques imaging spectroscopy, emission line [Quasars], Astronomy and Astrophysics, evolution [Galaxies], individual: PDS 456 [Quasars], Astrophysics - Astrophysics of Galaxies, galaxies evolution, Interstellar medium, quasars: emission lines, Stars, Radiation pressure, 13. Climate action, Space and Planetary Science, techniques interferometric, techniques: imaging spectroscopy, techniques: interferometric, Astrophysics of Galaxies (astro-ph.GA), interferometric [Techniques], Outflow, quasars emission line, galaxies: evolution
Abstract: We report on the first ALMA observation of the CO(3$-$2) and rest-frame ~340 GHz continuum emission in PDS 456, which is the most luminous, radio-quiet QSO in the local Universe ($z$~0.18), with a bolometric luminosity $L_{\rm Bol}\sim10^{47}$ erg s$^{-1}$. ALMA angular resolution allowed us to map scales as small as ~700 pc. The molecular gas reservoir, traced by the core of the very bright CO(3$-$2) emission line, is distributed in a compact rotating disk, with size of ~1.3 kpc, seen close to face-on ($i$~25 deg). Fast CO(3$-$2) emission in the velocity range $v\in[-1000,+500]$ km s$^{-1}$ is also present. Specifically, we detect several blue-shifted clumps out to ~5 kpc from the nucleus, in addition to a compact ($R\lesssim1.2$ kpc), broad emission component. These components reveal a galaxy-wide molecular outflow, with a total mass $M_{\rm mol}^{\rm out}\sim2.5\times10^8$ $M_{\odot}$ and a mass outflow rate $\dot{M}_{\rm mol}\sim290$ $M_{\odot}$ yr$^{-1}$. The corresponding depletion time is ~8 Myr, shorter than the rate at which the molecular gas is converted into stars, indicating that the detected outflow is potentially able to quench star-formation in the host. The momentum flux of the molecular outflow normalised to the radiative momentum output (i.e. $L_{\rm Bol}/c$) is $\lesssim1$, comparable to that of the X-ray ultra-fast outflow (UFO) detected in PDS 456. This is at odds with the expectations for an energy-conserving expansion suggested for most of the large-scale outflows detected in low-luminosity AGN so far. We suggest three possible scenarios that may explain this observation: (i) in very luminous AGN such as our target the molecular gas phase is tracing only a fraction of the total outflowing mass; (ii) a small coupling between the shocked gas by the UFO and the host-galaxy ISM (iii) AGN radiation pressure may play an important role in driving the outflow., Accepted in A&A
Published: 2019

27. Connecting X-ray nuclear winds with galaxy-scale ionised outflows in two z ∼ 1.5 lensed quasars

Author: M. Mingozzi, Giovanni Cresci, A. Marconi, Vincenzo Mainieri, A. Marasco, Michele Perna, Giacomo Venturi, Giorgio Lanzuisi, M. Dadina, G. Chartas, Andrea Comastri, A. Amiri, F. Rizzo, F. Mannucci, C. Vignali, G. Tozzi, E. Nardini, Marcella Brusa, Tozzi, G. [0000-0003-4226-7777], Cresci, G. [0000-0002-5281-1417], Marasco, A. [0000-0002-5655-6054], Nardini, E. [0000-0001-9226-8992], Marconi, A. [0000-0002-9889-4238], Mannucci, F. [0000-0002-4803-2381], Rizzo, F. [0000-0001-9705-2461], Amiri, A. [0000-0002-8553-1964], Dadina, M. [0000-0002-7858-7564], Lanzuisi, G. [0000-0001-9094-0984], Mainieri, V. [0000-0002-1047-9583], Mingozzi, M. [0000-0003-2589-762X], Perna, M. [0000-0002-0362-5941], Venturi, G. [0000-0001-8349-3055], Italian Ministry for University and Research (MUR), Agencia Estatal de Investigación (AEI), Comunidad de Madrid, Tozzi, G., Cresci, G., Marasco, A., Nardini, E., Marconi, A., Mannucci, F., Chartas, G., Rizzo, F., Amiri, A., Brusa, M., Comastri, A., Dadina, M., Lanzuisi, G., Mainieri, V., Mingozzi, M., Perna, M., Venturi, G., and Vignali, C.
Subjects: Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Doubly ionized oxygen, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Momentum, emission lines [Quasars], 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, jets and outflows [ISM], 010308 nuclear & particles physics, imaging spectroscopy [Techniques], Astronomy and Astrophysics, Quasar, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: evolution – quasars: emission lines – ISM: jets and outflows – techniques: imaging spectroscopy – galaxies: active, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow
Abstract: Outflows driven by active galactic nuclei (AGN) are expected to have a significant impact on the host galaxy evolution, but it is still debated how they are accelerated and propagate on galaxy-wide scales. This work addresses these questions by studying the link between X-ray, nuclear ultra-fast outflows (UFOs) and extended ionised outflows, for the first time in two quasars close to the peak of AGN activity ($z\sim2$), where AGN feedback is expected to be more effective. As targets, we selected two multiple-lensed quasars at $z\sim1.5$, HS 0810+2554 and SDSS J1353+1138, known to host UFOs and observed with the near-IR integral field spectrometer SINFONI at the VLT. We performed a kinematical analysis of the [O III]$\lambda$5007 optical emission line, in order to trace the presence of ionised outflows. We detected spatially resolved ionised outflows in both galaxies, extended more than 8 kpc and moving up to $v>2000$ km/s. We derived mass outflow rates of $\sim$12 M$_{sun}$/yr and $\sim$2 M$_{sun}$/yr for HS 0810+2554 and SDSS J1353+1138. Comparing with the co-hosted UFO energetics, the ionised outflow energetics in HS 0810+2554 is broadly consistent with a momentum-driven regime of wind propagation, while in SDSS J1353+1138 it differs by a factor of $\sim$100 from theoretical predictions, requiring either a massive molecular outflow or a high variability of the AGN activity to account for such a discrepancy. By additionally considering our results with those from the small sample of well-studied objects (all local but one), with both UFO and extended (ionised/atomic/molecular) outflow detections, we found that in 10 out of 12 galaxies the large-scale outflow energetics is consistent with the theoretical predictions of either a momentum- or an energy-driven scenario. This suggests that such models explain relatively well the acceleration mechanism of AGN-driven winds on large scales., Comment: 19 pages, 9 figures. Accepted for publication in A&A
Published: 2021

28. SUPER I. Toward an unbiased study of ionized outflows in z~2 active galactic nuclei: survey overview and sample characterization

Author: G. Rodighiero, Luca Zappacosta, Alessandra Lamastra, Chiara Feruglio, S. Carniani, Paolo Padovani, Enrico Piconcelli, Giovanni Cresci, Michele Perna, Andreas Schulze, Claudia Cicone, Mara Salvato, D. Kakkad, Bernd Husemann, M. Bischetti, John D. Silverman, Angela Bongiorno, B. Balmaverde, Andrea Merloni, Alessandro Marconi, C. Circosta, Francesca Civano, Alexander Karim, Fabrizio Fiore, M. Schramm, Alfio Puglisi, C. Vignali, G. Zamorani, Giorgio Lanzuisi, Vincenzo Mainieri, Benjamin Magnelli, Eva Schinnerer, G. Vietri, Andrea Comastri, Hagai Netzer, Sotiria Fotopoulou, Christopher Harrison, F. Mannucci, Marcella Brusa, Circosta, C., Mainieri, V., Padovani, P., Lanzuisi, G., Salvato, M., Harrison, C. M., Kakkad, D., Puglisi, A., Vietri, G., Zamorani, G., Cicone, C., Husemann, B., Vignali, C., Balmaverde, B., Bischetti, M., Bongiorno, A., Brusa, M., Carniani, S., Civano, F., Comastri, A., Cresci, G., Feruglio, C., Fiore, F., Fotopoulou, S., Karim, A., Lamastra, A., Magnelli, B., Mannucci, F., Marconi, A., Merloni, A., Netzer, H., Perna, M., Piconcelli, E., Rodighiero, G., Schinnerer, E., Schramm, M., Schulze, A., Silverman, J., Zappacosta, L., DEU, and Circosta C., Mainieri V, Padovani P., Lanzuisi G., Salvato M., Harrison C. M., Kakkad D., Puglisi A., Vietri G., Zamorani G., Cicone C., Husemann B., Vignali C., Balmaverde B., Bischetti M., Bongiorno A., Brusa M., Carniani S., Civano F., Comastri A., Cresci G., Feruglio C., Fiore F., Fotopoulou S., Karim A., Lamastra A., Magnelli B., Mannucci F., Marconi A., Merloni A., Netzer H., Perna M., Piconcelli E., Rodighiero G., Schinnerer E., Schramm M., Schulze A., Silverman J., Zappacosta L.
Subjects: Galaxies: Active, Galaxies: Evolution, Ism: Jets and outflows, Quasars: General, Surveys, Astronomy and Astrophysics, Space and Planetary Science, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General [Quasars], 01 natural sciences, Evolution [Galaxies], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Jets and outflow [Ism], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, alaxies: active, galaxies: evolution, quasars: general, surveys, ISM: jets and outflows, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Active [Galaxies], Photometry (astronomy), Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution
Abstract: Theoretical models of galaxy formation suggest that the presence of an active galactic nucleus (AGN) is required to regulate the growth of its host galaxy through feedback mechanisms, produced by e.g. AGN-driven outflows. Although such outflows are common both at low and high redshift, a comprehensive picture is still missing. The peak epoch of galaxy assembly (1, Comment: 28 pages, 8 figures, 5 tables. Accepted for publication in A&A
Published: 2018

29. Molecular outflow and feedback in the obscured quasar XID2028 revealed by ALMA

Author: Emanuele Daddi, Filippo Fraternali, Rosita Paladino, Lorenzo Busoni, Paola Santini, Dieter Lutz, Marcella Brusa, Michele Perna, Mark Sargent, Giorgio Lanzuisi, Giovanni Cresci, Andrea Comastri, Alessandro Marconi, Sebastian Rabien, Fabrizio Fiore, Francesco Di Vito, Filippo Mannucci, Chiara Feruglio, Iskren Y. Georgiev, A. Bongiorno, N. Z. Scoville, Stefano Carniani, Marco Bonaglia, Enrico Piconcelli, Cristian Vignali, F. Duras, G. Zamorani, F. La Franca, Elisabeta Lusso, Viviana Casasola, Roberto Gilli, V. Mainieri, Brusa, M., Cresci, G., Daddi, E., Paladino, R., Perna, MARIA FRANCESCA, Bongiorno, A., Lusso, E., Sargent, M. T., Casasola, V., Feruglio, C., Fraternali, Fabrizio, Georgiev, I., Mainieri, V., Carniani, S., Comastri, A., Duras, F., Fiore, F., Mannucci, F., Marconi, A., Piconcelli, E., Zamorani, G., Gilli, R., La Franca, F., Lanzuisi, G., Lutz, D., Santini, P., Scoville, N. Z., Vignali, C., DI VITO, Francesco, Rabien, S., Busoni, L., Bonaglia, M., Brusa M., Cresci G., Daddi E. , Paladino R., Perna M., Bongiorno A., Lusso E., Sargent M. T., Casasola V., Feruglio C., Fraternali F. , Georgiev I., Mainieri V., Carniani S., Comastri A., Duras F., Fiore F., Mannucci F., Marconi A., Piconcelli E., Zamorani G., Gilli R., La Franca F., Lanzuisi G., Lutz D., Santini P., Scoville N. Z., Vignali C., Vito F. , Rabien S., Busoni L., Bonaglia M., Perna, M., Fraternali, F., Vito, F., Carniani, Stefano [0000-0002-6719-380X], Apollo - University of Cambridge Repository, ITA, USA, GBR, FRA, and DEU
Subjects: active [Galaxies], galaxies: active, Doubly ionized oxygen, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, star formation [Galaxies], quasars: individual: XID2028, Settore FIS/05 - Astronomia e Astrofisica, Coincident, 0103 physical sciences, ISM [Galaxies], 010303 astronomy & astrophysics, quasars, galaxies, ISM, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Sigma, Astronomy and Astrophysics, Quasar, Plasma, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Outflow, individual: XID2028 [Quasars], Excitation, galaxies: ISM
Abstract: We imaged, with ALMA and ARGOS/LUCI, the molecular gas and dust and stellar continuum in XID2028, which is an obscured quasi-stellar object (QSO) at z = 1.593, where the presence of a massive outflow in the ionised gas component traced by the [OIII]5007 emission has been resolved up to 10 kpc. This target represents a unique test case to study QSO feedback in action at the peak epoch of AGN-galaxy co-evolution. The QSO was detected in the CO(5 − 4) transition and in the 1.3 mm continuum at ~30 and ~20σ significance, respectively; both emissions are confined in the central (, Includes STFC and ERC grants.
Published: 2018

30. The MAGNUM survey: positive feedback in the nuclear region of NGC 5643 suggested by MUSE

Author: Giacomo Venturi, Roberto Maiolino, Filippo Mannucci, Chiara Feruglio, Mara Salvato, Paolo Tozzi, Joss Bland-Hawthorn, Stefano Zibetti, Alessandro Capetti, Guido Risaliti, Giovanni Cresci, Tohru Nagao, Claudia Cicone, Eleonora Sani, Alessandro Marconi, Stefano Carniani, Barbara Balmaverde, Marcella Brusa, Ernesto Oliva, Anna Gallazzi, Tanya Urrutia, ITA, Cresci, G, Marconi, A., Zibetti, S., Risaliti, G., Carniani, S., Mannucci, F., Gallazzi, A., Maiolino, R., Balmaverde, B., Brusa, M., Capetti, A., Cicone, C., Feruglio, C., Bland-Hawthorn, J., Nagao, T., Oliva, E., Salvato, M., Sani, E., Tozzi, P., Urrutia, T., Venturi, G., and Cresci, G.
Subjects: Galaxies: individual: NGC 5643, Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Settore FIS/05 - Astronomia e Astrofisica, Ionization, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Techniques: imaging spectroscopy, ISM: jets and outflow, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, individual: NGC 5643 [Galaxies], Star formation, imaging spectroscopy [Techniques], jets and outflow [ISM], Astronomy and Astrophysics, Galaxies: active, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Dust lane, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract: We study the ionization and kinematics of the ionized gas in the nuclear region of the barred Seyfert 2 galaxy NGC~5643 using MUSE integral field observations in the framework of the MAGNUM (Measuring Active Galactic Nuclei Under MUSE Microscope) survey. The data were used to identify regions with different ionization conditions and to map the gas density and the dust extinction. We find evidence for a double sided ionization cone, possibly collimated by a dusty structure surrounding the nucleus. At the center of the ionization cone, outflowing ionized gas is revealed as a blueshifted, asymmetric wing of the [OIII] emission line, up to projected velocity v(10)~-450 km/s. The outflow is also seen as a diffuse, low luminosity radio and X-ray jet, with similar extension. The outflowing material points in the direction of two clumps characterized by prominent line emission with spectra typical of HII regions, located at the edge of the dust lane of the bar. We propose that the star formation in the clumps is due to `positive feedback' induced by gas compression by the nuclear outflow, providing the first candidate for outflow induced star formation in a Seyfert-like radio quiet AGN. This suggests that positive feedback may be a relevant mechanism in shaping the black hole-host galaxy coevolution., Comment: 9 pages, 7 figures, accepted for publication in A&A
Published: 2015

31. X-shooter reveals powerful outflows in z~1.5 X-ray selected obscured quasi stellar objects

Author: Alessandro Marconi, Fabrizio Fiore, Angela Bongiorno, Giorgio Lanzuisi, David J. Rosario, Michele Perna, Dieter Lutz, Marcella Brusa, Andrea Comastri, Giovanni Cresci, Roberto Gilli, Roberto Maiolino, Andrea Merloni, Mara Salvato, Elisabeta Lusso, C. Vignali, Francesca Onori, G. Zamorani, F. La Franca, Vincenzo Mainieri, P. Santini, M. Mignoli, Enrico Piconcelli, ITA, USA, Brusa, M., Bongiorno, A., Cresci, G., Perna, M., Marconi, A., Mainieri, V., Maiolino, R., Salvato, M., Lusso, E., Santini, P., Comastri, A., Fiore, F., Gilli, R., Franca, F. L., Lanzuisi, G., Lutz, D., Merloni, A., Mignoli, M., Onori, F., Piconcelli, E., Rosario, D., Vignali, C., Zamorani, G., Brusa, M, Bongiorno, A, Cresci, G, Perna, M, Marconi, A, Mainieri, V, Maiolino, R, Salvato, M, Lusso, E, Santini, P, Comastri, A, Fiore, F, Gilli, R, LA FRANCA, Fabio, Lanzuisi, G, Lutz, D, Merloni, A, Mignoli, M, Onori, F, Piconcelli, E, Rosario, D, and Vignali, C
Subjects: QSOS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, galaxies active, galaxies evolution, quasars emission lines, quasars supermassive black holes, cosmology observations, Young stellar object, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Luminosity, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, quasars: supermassive black hole, Astrophysics::Galaxy Astrophysics, Photometric redshift, Luminous infrared galaxy, Physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, galaxies: evolution, quasars: emission line, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present X-shooter at the Vewry Large Telescope observations of a sample of 10 luminous, X-ray obscured QSOs at z$\sim1.5$ from the XMM-COSMOS survey, expected to be caught in the transitioning phase from starburst to active galactic nucleus (AGN)-dominated systems. The main selection criterion is X-ray detection at bright fluxes (L$>=10^{44}$ erg s$^{-1}$) coupled to red optical-to-NIR-to-MIR colors. Thanks to its large wavelength coverage, X-shooter allowed us to determine accurate redshifts from the presence of multiple emission lines for five out of six targets for which we had only a photometric redshift estimate, with an 80 percent success rate, significantly larger than what is observed in similar programs of spectroscopic follow-up of red QSOs. We report the detection of broad and shifted components in the [OIII]$\lambda\lambda$5007,4959 complexes for six out of eight sources with these lines observable in regions free from strong atmospheric absorptions. The full width half-maximum (FWHM) associated with the broad components are in the range FWHM$\sim900-1600$ km s$^{-1}$, larger than the average value observed in SDSS Type 2 AGN samples at similar observed [OIII] luminosity, but comparable to those observed for QSO/ultraluminous infrared galaxies systems for which the presence of kpc scale outflows have been revealed through integral field unit spectroscopy. Although the total outflow energetics (inferred under reasonable assumptions) may be consistent with winds accelerated by stellar processes, we favour an AGN origin for the outflows given the high outflow velocities oberved (v$>1000$ km s$^{-1}$) and the presence of strong winds also in objects undetected in the far infrared., Comment: Final version to appear in MNRAS (lower limits added in Figure 9 and additional 3 spectra added in the appendix; results unchanged)
Published: 2014

32. Dynamical properties of AMAZE and LSD galaxies from gas kinematics and the Tully-Fisher relation at z~3

Author: Andrea Cimatti, A. Gnerucci, Francesca Matteucci, Andrea Grazian, Roberto Maiolino, Filippo Mannucci, Francesco Calura, Lucia Pozzetti, F. Cocchia, Alessandro Marconi, Giovanni Cresci, Tohru Nagao, P. Troncoso, Gnerucci A., Marconi A., Cresci G., Maiolino R., Mannucci F., Calura F., Cimatti A., Cocchia F., Grazian A., Matteucci F., Nagao T., Pozzetti L., Troncoso P., Gnerucci, A., Marconi, A., Cresci, G., Maiolino, R., Mannucci, F., Calura, F., Cimatti, A., Cocchia, F., Grazian, A., Matteucci, MARIA FRANCESCA, Nagao, T., Pozzetti, L., and Troncoso, P.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], Field (physics), Metallicity, FOS: Physical sciences, Angular velocity, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, Tully–Fisher relation, 01 natural sciences, galaxies: evolution, galaxies: formation, galaxies: fundamental parameters, galaxies: high-redshift, galaxies: kinematics and dynamics, kinematics and dynamics [galaxies], 0103 physical sciences, 010303 astronomy & astrophysics, evolution [galaxies], galaxies: fundamental parameter, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, fundamental parameter [galaxies], Velocity dispersion, Astronomy and Astrophysics, Galaxy, Baryon, Space and Planetary Science, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a SINFONI integral field kinematical study of 33 galaxies at z~3 from the AMAZE and LSD projects which are aimed at studying metallicity and dynamics of high-redshift galaxies. The number of galaxies analyzed in this paper constitutes a significant improvement compared to existing data in the literature and this is the first time that a dynamical analysis is obtained for a relatively large sample of galaxies at z~3. 11 galaxies show ordered rotational motions (~30% of the sample), in these cases we estimate dynamical masses by modeling the gas kinematics with rotating disks and exponential mass distributions. We find dynamical masses in the range 2 \times 10^9 M\odot - 2 \times 10^11 M\odot with a mean value of ~ 2 \times 10^10 M\odot. By comparing observed gas velocity dispersion with that expected from models, we find that most rotating objects are dynamically "hot", with intrinsic velocity dispersions of the order of ~90 km s-1. The median value of the ratio between the maximum disk rotational velocity and the intrinsic velocity dispersion for the rotating objects is 1.6, much lower than observed in local galaxies value (~10) and slightly lower than the z~2 value (2 - 4). Finally we use the maximum rotational velocity from our modeling to build a baryonic Tully-Fisher relation at z~3. Our measurements indicate that z~3 galaxies have lower stellar masses (by a factor of ten on average) compared to local galaxies with the same dynamical mass. However, the large observed scatter suggests that the Tully-Fisher relation is not yet "in place" at these early cosmic ages, possibly due to the young age of galaxies. A smaller dispersion of the Tuly-Fisher relation is obtained by taking into account the velocity dispersion with the use of the S_0.5 indicator, suggesting that turbulent motions might have an important dynamical role., A&A accepted
Published: 2010

33. The VANDELS survey: a strong correlation between Ly α equivalent width and stellar metallicity at 3 ≤ z ≤ 5

Author: A. Calabrò, O. Cucciati, G. Zamorani, D. J. McLeod, Ross J. McLure, Nimish P. Hathi, Lucia Guaita, B. Garilli, James Dunlop, Johan P. U. Fynbo, Laura Pentericci, Mauro Giavalisco, Marco Castellano, Margherita Talia, Andrea Cimatti, Fergus Cullen, Adriano Fontana, M. Bolzonella, A. Saxena, Ricardo Amorín, Giovanni Cresci, A. C. Carnall, F. Mannucci, Michele Cirasuolo, Fabio Fontanot, Matt J. Jarvis, Lucia Pozzetti, Anton M. Koekemoer, Alice E. Shapley, ITA, USA, GBR, FRA, DEU, Cullen, F, McLure, RJ, Dunlop, JS, Carnall, AC, McLeod, DJ, Shapley, AE, Amorin, R, Bolzonella, M, Castellano, M, Cimatti, A, Cirasuolo, M, Cucciati, O, Fontana, A, Fontanot, F, Garilli, B, Guaita, L, Jarvis, MJ, Pentericci, L, Pozzetti, L, Talia, M, Zamorani, G, Calabro, A, Cresci, G, Fynbo, JPU, Hathi, NP, Giavalisco, M, Koekemoer, A, Mannucci, F, and Saxena, A
Subjects: Physics, education.field_of_study, Stellar population, 010308 nuclear & particles physics, astro-ph.GA, Metallicity, Population, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Spectral line, galaxies: high-redshift, Space and Planetary Science, 0103 physical sciences, Spectral fitting, galaxies: evolution, education, 010303 astronomy & astrophysics, Equivalent width, evolution [galaxies], high-redshift [galaxies]
Abstract: We present the results of a new study investigating the relationship between observed Ly α equivalent width (Wλ(Ly α)) and the metallicity of the ionizing stellar population ( Z⋆) for a sample of 768 star-forming galaxies at 3 ≤ z ≤ 5 drawn from the VANDELS survey. Dividing our sample into quartiles of rest-frame Wλ(Ly α) across the range $-58 \,\rm {\mathring{\rm A}} \lesssim$ Wλ(Ly α) $\lesssim 110 \,\rm {\mathring{\rm A}}$ , we determine Z⋆ from full spectral fitting of composite far-ultraviolet spectra and find a clear anticorrelation between Wλ(Ly α) and Z⋆. Our results indicate that Z⋆ decreases by a factor ≳ 3 between the lowest Wλ(Ly α) quartile (λ(Ly α) $\rangle =-18\,\rm {\mathring{\rm A}}$ ) and the highest Wλ(Ly α) quartile (λ(Ly α) $\rangle =24\,\rm {\mathring{\rm A}}$ ). Similarly, galaxies typically defined as Lyman alpha emitters (LAEs; Wλ(Ly α) $\gt 20\,\rm {\mathring{\rm A}}$ ) are, on average, metal poor with respect to the non-LAE galaxy population (Wλ(Ly α) $\le 20\,\rm {\mathring{\rm A}}$ ) with Z⋆non-LAE ≳ 2 × Z⋆LAE. Finally, based on the best-fitting stellar models, we estimate that the increasing strength of the stellar ionizing spectrum towards lower Z⋆ is responsible for ${\simeq}15{-}25{{\ \rm per\ cent}}$ of the observed variation in Wλ(Ly α) across our sample, with the remaining contribution ( ${\simeq}75{-}85{{\ \rm per\ cent}}$ ) being due to a decrease in the H I/dust covering fractions in low- Z⋆ galaxies.
Published: 2020

34. The VANDELS survey: the stellar metallicities of star-forming galaxies at $\mathbf {2.5\,\, \lt\,\, z\,\, \lt\,\, 5.0}$

Author: Marco Castellano, Margherita Talia, Laura Pentericci, M. Bolzonella, Ross J. McLure, James Dunlop, Johan P. U. Fynbo, F. Marchi, Pascale Hibon, Ricardo Amorín, Fabio Fontanot, B. Garilli, Adriana Gargiulo, G. Zamorani, Lucia Guaita, D. J. McLeod, Fergus Cullen, Andrea Cimatti, Giovanni Cresci, A. C. Carnall, Romeel Davé, Lucia Pozzetti, Michele Cirasuolo, F. Mannucci, Nimish P. Hathi, Sadegh Khochfar, Alice E. Shapley, Cullen F., McLure R.J., Dunlop J.S., Khochfar S., Dave R., Amorin R., Bolzonella M., Carnall A.C., Castellano M., Cimatti A., Cirasuolo M., Cresci G., Fynbo J.P.U., Fontanot F., Gargiulo A., Garilli B., Guaita L., Hathi N., Hibon P., Mannucci F., Marchi F., McLeod D.J., Pentericci L., Pozzetti L., Shapley A.E., Talia M., and Zamorani G.
Subjects: Stellar mass, Stellar population, astro-ph.GA, Star (game theory), Metallicity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Galaxies: evolution, Order (ring theory), high redshift [galaxies], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxies: high redshift, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: We present the results of a study utilising ultra-deep, rest-frame UV, spectroscopy to quantify the relationship between stellar mass and stellar metallicity for 681 star-forming galaxies at $2.5, Comment: 21 pages (+ appendix), 13 figures, MNRAS accepted
Published: 2019

35. The NIRVANDELS Survey: a robust detection of α-enhancement in star-forming galaxies at z 3.4

Author: Naveen A. Reddy, Marco Castellano, G. Zamorani, Alice E. Shapley, Ross J. McLure, F. Mannucci, M. Bolzonella, A. Calabrò, Ricardo Amorín, Adriano Fontana, M. Hamadouche, Michele Cirasuolo, Nimish P. Hathi, Fergus Cullen, Michael W. Topping, James Dunlop, Ryan L. Sanders, L. Guaita, Fabio Fontanot, R. Begley, D. J. McLeod, Andrea Cimatti, Giovanni Cresci, A. C. Carnall, Laura Pentericci, Margherita Talia, A. Saxena, B. Garilli, Cullen F., Shapley A.E., McLure R.J., Dunlop J.S., Sanders R.L., Topping M.W., Reddy N.A., Amorin R., Begley R., Bolzonella M., Calabro A., Carnall A.C., Castellano M., Cimatti A., Cirasuolo M., Cresci G., Fontana A., Fontanot F., Garilli B., Guaita L., Hamadouche M., Hathi N.P., Mannucci F., McLeod D.J., Pentericci L., Saxena A., Talia M., and Zamorani G.
Subjects: Physics, 010308 nuclear & particles physics, astro-ph.GA, Star (game theory), Metallicity, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxies: high redshift, 01 natural sciences, Galaxy, Redshift, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxies: abundance
Abstract: We present results from the NIRVANDELS survey investigating the gas-phase metallicity ($\mathrm{Z}_{\mathrm{gas}}$, tracing O/H) and stellar metallicity ($Z_{\star}$, tracing Fe/H) of 33 star-forming galaxies at redshifts $2.95 < z < 3.80$. Based on a combined analysis of deep optical and near-IR spectra, tracing the rest-frame far ultraviolet and rest-frame optical respectively, we present the first simultaneous determination of the stellar and gas-phase mass-metallicity relationships (MZRs) at $z\simeq3.4$. In both cases, we find that metallicity increases with increasing stellar mass ($M_{\star}$), and that the power-law slope at $M_{\star} \lesssim 10^{10} \mathrm{M}_{\odot}$ of both MZRs scales as $Z \propto M_{\star}^{0.3}$. Comparing the stellar and gas-phase MZRs, we present direct evidence for super-solar O/Fe ratios (i.e., $\alpha$-enhancement) at $z>3$, finding $\mathrm{(O/Fe)}\simeq (2.54 \pm 0.38) \times \mathrm{(O/Fe)}_{\odot}$, with no clear dependence on $M_{\star}$., Comment: 18 pages, 11 figures, MNRAS accepted
Published: 2021

36. The VANDELS ESO public spectroscopic survey

Author: Nimish P. Hathi, Michele Moresco, Jennifer M. Lotz, Seock-Sam Kim, Lidia Tasca, Andrea Grazian, Intae Jung, Adriano Fontana, Casey Papovich, William G. Hartley, Kirpal Nandra, Emanuela Pompei, S. Bardelli, R. Begley, Mauro Giavalisco, Paola Santini, H. C. Ferguson, Andrea Cimatti, J. S. Dunlop, Lucia Guaita, H. Mendez-Hernandez, Christina C. Williams, Giovanni Cresci, A. C. Carnall, A. Saxena, Adriana Gargiulo, Paolo Cassata, A. Iovino, C. Caputi, D. Maccagni, Stephane Charlot, Michele Cirasuolo, Johan P. U. Fynbo, Stefano Cristiani, Fabrizio Fiore, L. Pentericci, Guido Roberts-Borsani, E. Curtis-Lake, M. Longhetti, Manuela Magliocchetti, Matt J. Jarvis, M. Mignoli, Y. Khusanova, Paola Popesso, Annalisa Citro, Mara Salvato, Ricardo Amorín, Lucia Pozzetti, Olga Cucciati, Fergus Cullen, Pascale Hibon, Fernando Buitrago, Daniel P. Stark, Corentin Schreiber, M. Fumana, P. Franzetti, Jairo Méndez-Abreu, E. Zucca, R. C. Thomas, Filippo Mannucci, Ross J. McLure, Mark Dickinson, K. Matsuoka, M. Franco, O. Le Fèvre, Daniel Schaerer, Steve Finkelstein, M. Bolzonella, Fabio Fontanot, David J. Rosario, Eric F. Bell, Marco Castellano, A. Calabrò, Antonis Georgakakis, Mario Nonino, G. Vietri, Maurilio Pannella, G. Brammer, Marcella Brusa, David T. Maltby, Stéphanie Juneau, Bianca Garilli, Anton M. Koekemoer, Angela Bongiorno, Vivienne Wild, Giovanni G. Fazio, David Elbaz, Margherita Talia, D. J. McLeod, M. Scodeggio, Alberto Saldana-Lopez, M. Hamadouche, Italo Balestra, Omar Almaini, G. Zamorani, Eros Vanzella, Rebecca A. A. Bowler, 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 Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Garilli B., McLure R., Pentericci L., Franzetti P., Gargiulo A., Carnall A., Cucciati O., Iovino A., Amorin R., Bolzonella M., Bongiorno A., Castellano M., Cimatti A., Cirasuolo M., Cullen F., Dunlop J., Elbaz D., Finkelstein S., Fontana A., Fontanot F., Fumana M., Guaita L., Hartley W., Jarvis M., Juneau S., Maccagni D., McLeod D., Nandra K., Pompei E., Pozzetti L., Scodeggio M., Talia M., Calabro A., Cresci G., Fynbo J.P.U., Hathi N.P., Hibon P., Koekemoer A.M., Magliocchetti M., Salvato M., Vietri G., Zamorani G., Almaini O., Balestra I., Bardelli S., Begley R., Brammer G., Bell E.F., Bowler R.A.A., Brusa M., Buitrago F., Caputi C., Cassata P., Charlot S., Citro A., Cristiani S., Curtis-Lake E., Dickinson M., Fazio G., Ferguson H.C., Fiore F., Franco M., Georgakakis A., Giavalisco M., Grazian A., Hamadouche M., Jung I., Kim S., Khusanova Y., Le Fevre O., Longhetti M., Lotz J., Mannucci F., Maltby D., Matsuoka K., Mendez-Hernandez H., Mendez-Abreu J., Mignoli M., Moresco M., Nonino M., Pannella M., Papovich C., Popesso P., Roberts-Borsani G., Rosario D.J., Saldana-Lopez A., Santini P., Saxena A., Schaerer D., Schreiber C., Stark D., Tasca L.A.M., Thomas R., Vanzella E., Wild V., Williams C., Zucca E., University of St Andrews. School of Physics and Astronomy, and 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)
Subjects: SELECTION, Galaxies: fundamental parameter, Astrophysics, I, Surveys, 01 natural sciences, observations/surveys/catalogs [Cosmology], Cosmology: observation, Cosmology: Observations, Spectral line, statistics [Galaxies], DATA-REDUCTION, QB Astronomy, Galaxies: distances and redshift, Galaxies: Fundamental Parameters, 010303 astronomy & astrophysics, QC, QB, REDSHIFT SURVEY, Physics, observations [cosmology], Catalogs, Cosmology: observations, Galaxies: distances and redshifts, Galaxies: fundamental parameters, Galaxies: statistics, Galaxies: Statistics, fundamental parameters [Galaxies], astro-ph.CO, Catalog, X-RAY-PROPERTIES, Data release, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: Distances and Redshifts, surveys, 0103 physical sciences, STAR-FORMING GALAXIES, distances and redshifts [Galaxies], Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Galaxies: statistic, Astronomy and Astrophysics, DAS, VLT DEEP SURVEY, Astrophysics - Astrophysics of Galaxies, EVOLUTION, STELLAR, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), QUIESCENT GALAXIES, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract: VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high signal to noise, medium resolution spectra of galaxies at redshift between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We give a detailed description of sample selection, observations and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at iAB = 25. The high Signal to Noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5�� allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-IR photometry and physical parameters derived through SED fitting. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range 8.3< Log(M*/Msolar), 16 pages, 13 figures, accepted for publication in Astronomy & Astrophysics
Published: 2021

37. The evolution of the mass-metallicity relations from the VANDELS survey and the GAEA Semi-Analytic model

Author: Johan P. U. Fynbo, Pascale Hibon, Gabriella De Lucia, Filippo Mannucci, Ricardo Amorín, Margherita Talia, R. J. McLure, A. Calabrò, O. Cucciati, M. Castellano, Lucia Pozzetti, Angela Bongiorno, Nimish P. Hathi, Fergus Cullen, Fabio Fontanot, Anna Gallazzi, Michaela Hirschmann, Lizhi Xie, Laura Pentericci, Micol Bolzonella, Giovanni Cresci, Fontanot F., Calabro A., Talia M., Mannucci F., Castellano M., Cresci G., De Lucia G., Gallazzi A., Hirschmann M., Pentericci L., Xie L., Amorin R., Bolzonella M., Bongiorno A., Cucciati O., Cullen F., Fynbo J.P.U., Hathi N., Hibon P., McLure R.J., and Pozzetti L.
Subjects: SPECTROSCOPIC SURVEY, Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], Stellar mass, Metallicity, CONSISTENT, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, abundances [galaxies], STAR-FORMING GALAXIES, SPECTRA, galaxies: formation, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, Star formation, CANDELS, Analytic model, Astronomy and Astrophysics, CHEMICAL ABUNDANCES, Astrophysics - Astrophysics of Galaxies, AGES, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), STELLAR MASS, galaxies: evolution, NEBULAE, galaxies: Abundance, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In this work, we study the evolution of the mass-metallicity relations (MZRs) as predicted by the GAlaxy Evolution and Assembly (GAEA) semi-analytic model. We contrast these predictions with recent results from the VANDELS survey, that allows us to expand the accessible redshift range for the stellar MZR up to $z\sim3.5$. We complement our study by considering the evolution of the gas-phase MZR in the same redshift range. We show that GAEA is able to reproduce the observed evolution of the $z, 12 pages, 8 figures, MNRAS accepted, replaced to match the published version
Published: 2021
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38. Turbulence/outflows perpendicular to low-power jets in Seyfert galaxies

Author: Filippo Mannucci, Giacomo Venturi, Matilde Mingozzi, Giovanni Cresci, A. Marconi, S. Carniani, T. Storchi-Bergmann, W. Forman, R. Overzier, R. Riffel, Venturi, G., Marconi, A., Mingozzi, M., Cresci, G., Carniani, S., and Mannucci, F.
Subjects: Physics, Jet (fluid), Active galactic nucleus, 010308 nuclear & particles physics, Turbulence, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Integral field spectrograph, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Ionization, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: We present recent results from our MAGNUM survey of nearby active galactic nuclei (AGN), which exploits observations from the optical/near-IR integral field spectrograph MUSE at VLT. We detect strongly enhanced line widths in emission line maps of four galaxies perpendicularly to their low-power jets and AGN ionisation cones, indicative of turbulent/outflowing material. The observation of a similar phenomenon in other works suggests that it originates from an interaction mechanism between the jet and the galaxy disc through which it propagates.
Published: 2021

39. Less and more IGM-transmitted galaxies from z ∼ 2.7 to z ∼ 6 from VANDELS and VUDS

Author: E. Zucca, J. P. U. Fynbo, Margherita Talia, Ricardo Amorín, Anton M. Koekemoer, Y. Khusanova, Stefano Cristiani, Pascale Hibon, Laura Pentericci, Marco Castellano, F. Mannucci, Daniel Schaerer, S. Bardelli, V. Le Brun, Andrea Cimatti, R. Thomas, B. Garilli, M. Franco, O. Le Fevre, Adriana Gargiulo, Giovanni Cresci, Fabio Fontanot, Nimish P. Hathi, Brian C. Lemaux, G. Zamorani, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), 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), 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), Thomas R., Pentericci L., Le Fevre O., Koekemoer A.M., Castellano M., Cimatti A., Fontanot F., Gargiulo A., Garilli B., Talia M., Amorin R., Bardelli S., Cristiani S., Cresci G., Franco M., Fynbo J.P.U., Hathi N.P., Hibon P., Khusanova Y., Le Brun V., Lemaux B.C., Mannucci F., Schaerer D., Zamorani G., and Zucca E.
Subjects: Physics, 0303 health sciences, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: miscellaneou, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, 03 medical and health sciences, Space and Planetary Science, galaxies: high-redshift, Intergalactic medium, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, intergalactic medium, cosmology: miscellaneous, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 030304 developmental biology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aim. Our aim is to analyse the variance of the Inter-Galactic Medium transmission (IGM) by studying this parameter in the rest-frame UV spectra of a large sample of high redshift galaxies. Method. We make use of the VIMOS Ultra Deep Survey and the VANDELS public survey to have an insight into the far UV spectrum of $2.7, Comment: Accepted for publication on A&A
Published: 2021

40. SUPER II. Spatially resolved ionised gas kinematics and scaling relations in z ∼ 2 AGN host galaxies

Author: Fabrizio Fiore, Giovanni Cresci, Annagrazia Puglisi, Luca Zappacosta, F. Mannucci, C. Cicone, C. Circosta, Chiara Feruglio, Vincenzo Mainieri, Alessandro Marconi, Enrico Piconcelli, D. Kakkad, Giorgio Lanzuisi, Bernd Husemann, Jakub Scholtz, G. Vietri, Andrea Comastri, Mara Salvato, M. Schramm, C. Vignali, Christopher Harrison, Nicola Menci, Michele Perna, G. Zamorani, Hagai Netzer, Paolo Padovani, Marcella Brusa, S. Carniani, John D. Silverman, M. Bischetti, Kakkad, D. [0000-0002-2603-2639], Manieri, V. [0000-0002-1047-9583], Vietri, G. [0000-0001-9155-8875], Carniani, S. [0000-0002-6719-380X], Perna, M. [0000-0002-0362-5941], Creci, G. [0000-0002-5281-1417], Husemann, B. [0000-0003-2901-6842], Bischetti, M. [0000-0002-4314-021X], Fiore, F. [0000-0002-4031-4157], Marconi, A. [0000-0002-9889-4238], Padovani, P. [0000-0002-4707-6841], Cicone, C. [0000-0003-0522-6941], Comastri, A. [0000-0003-3451-9970], Mannucci, F. [0000-0002-4803-2381], ESO program, 196.A-0377, Comunidad de Madrid, Kakkad, D., Mainieri, V., Vietri, G., Carniani, S., Harrison, C.M., Perna, M., Scholtz, J., Circosta, C., Cresci, G., Husemann, B., Bischetti, M., Feruglio, C., Fiore, F., Marconi, A., Padovani, P., Brusa, M., Cicone, C., Comastri, A., Lanzuisi, G., Mannucci, F., Menci, N., Netzer, H., Piconcelli, E., Puglisi, A., Salvato, M., Schramm, M., Silverman, J., Vignali, C., Zamorani, G., Zappacosta, L., Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, and Harrison, C. M.
Subjects: quasars emission lines, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, galaxies active, Doubly ionized oxygen, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, emission lines [Quarsars], 01 natural sciences, Luminosity, symbols.namesake, galaxies: high-redshift, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, galaxies high-redshift, 010308 nuclear & particles physics, Star formation, techniques imaging spectroscopy, imaging spectroscopy [Techniques], Balmer series, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, galaxies evolution, Galaxy, Active [Galaxies], Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics of Galaxies (astro-ph.GA), symbols, high redshift [Galaxies], galaxies: evolution, quasars: emission line
Abstract: The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) aims at tracing and characterizing ionized gas outflows and their impact on star formation in a statistical sample of X-ray selected Active Galactic Nuclei (AGN) at z$\sim$2. We present the first SINFONI results for a sample of 21 Type-1 AGN spanning a wide range in bolometric luminosity (log $\mathrm{L_{bol}}$ = 45.4-47.9 erg/s). The main aims of this paper are determining the extension of the ionized gas, characterizing the occurrence of AGN-driven outflows, and linking the properties of such outflows with those of the AGN. We use Adaptive Optics-assisted SINFONI observations to trace ionized gas in the extended narrow line region using the [OIII]5007 line. We classify a target as hosting an outflow if its non-parametric velocity of the [OIII] line, $\mathrm{w_{80}}$, is larger than 600 km/s. We study the presence of extended emission using dedicated point-spread function (PSF) observations, after modelling the PSF from the Balmer lines originating from the Broad Line Region. We detect outflows in all the Type-1 AGN sample based on the $\mathrm{w_{80}}$ value from the integrated spectrum, which is in the range 650-2700 km/s. There is a clear positive correlation between $\mathrm{w_{80}}$ and the AGN bolometric luminosity (99% correlation probability), but a weaker correlation with the black hole mass (80% correlation probability). A comparison of the PSF and the [OIII] radial profile shows that the [OIII] emission is spatially resolved for $\sim$35% of the Type-1 sample and the outflows show an extension up to $\sim$6 kpc. The relation between maximum velocity and the bolometric luminosity is consistent with model predictions for shocks from an AGN driven outflow. The escape fraction of the outflowing gas increase with the AGN luminosity, although for most galaxies, this fraction is less than 10%., Accepted for publication in A&A, 34 pages, 14 figures and 5 tables
Published: 2020

41. Linking the small scale relativistic winds and the large scale molecular outflows in the z = 1.51 lensed quasar HS 0810+2554

Author: Mauro Dadina, E. Davidson, Marcella Brusa, Massimo Cappi, C. Vignali, Giorgio Lanzuisi, Andrea Comastri, Rosita Paladino, George Chartas, Giovanni Cresci, Chartas, G., Davidson, E., Brusa, M., Vignali, C., Cappi, M., Dadina, M., Cresci, G., Paladino, R., Lanzuisi, G., and Comastri, A.
Subjects: Momentum flux, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Submillimeter Array, galaxies: high-redshift, quasars: general, 0103 physical sciences, High spatial resolution, Emission spectrum, ISM: jets and outflow, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, quasars: individual: HS 0810+2554, gravitational lensing: strong, Astronomy and Astrophysics, Quasar, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, Outflow
Abstract: We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the quadruply lensed z=1.51 quasar HS 0810+2554 which provide useful insight on the kinematics and morphology of the CO molecular gas and the ~2 mm continuum emission in the quasar host galaxy. Lens modeling of the mm-continuum and the spectrally integrated CO(3-2) images indicates that the source of the mm-continuum has an eccentricity of e~0.9 with a size of ~1.6 kpc and the source of line emission has an eccentricity of e~0.7 with a size of ~1 kpc. The spatially integrated emission of the CO(2-1) and CO(3-2) lines shows a triple peak structure with the outer peaks separated by Dv_21 = 220 +\- 19 km s^-1 and Dv_32 = 245 +/- 28 km s^-1, respectively, suggesting the presence of rotating molecular CO line emitting gas. Lensing inversion of the high spatial resolution images confirms the presence of rotation of the line emitting gas. Assuming a conversion factor of alpha_CO = 0.8 M_solar (K km s^-1 pc^2)^-1 we find the molecular gas mass of HS 0810+2554 to be M _ Mol = [(5.2 +/- 1.5)/mu_32] x10^10 M_solar, where mu_32 is the magnification of the CO(3-2) emission. We report the possible detection, at the 3.0 - 4.7 sigma confidence level, of shifted CO(3-2) emission lines of high-velocity clumps of CO emission with velocities up to 1702 km s^-1. We find that the momentum boost of the large scale molecular wind is below the value predicted for an energy-conserving outflow given the momentum flux observed in the small scale ultrafast outflow., Comment: 17 pages, includes 15 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society
Published: 2020
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42. SUPER

Author: Enrico Piconcelli, Michele Perna, D. Kakkad, G. Vietri, C. Circosta, V. Mainieri, Filippo Mannucci, F. Arrigoni Battaia, Christopher Harrison, Annagrazia Puglisi, Cristian Vignali, Stefano Carniani, Luca Zappacosta, Giovanni Cresci, Alessandro Marconi, Jakub Scholtz, G. Zamorani, C. Cicone, M. Bischetti, Cicone, C., Mainieri, V., Circosta, C., Kakkad, D., Vietri, G., Perna, M., Bischetti, Manuela, Carniani, S., Cresci, Giovanni, Harrison, C., Mannucci, Filippo, Marconi, Alessandro, Piconcelli, Enrico, Puglisi, A., Scholtz, J., Vignali, C., Zamorani, G., Zappacosta, Luca, Arrigoni Battaia, F., Cicone C., Mainieri V., Circosta C., Kakkad D., Vietri G., Perna M., Bischetti M., Carniani S., Cresci G., Harrison C., Mannucci F., Marconi A., Piconcelli E., Puglisi A., Scholtz J., Vignali C., Zamorani G., Zappacosta L., and Arrigoni Battaia F.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), halo [galaxies], galaxies: halos, FOS: Physical sciences, galaxies [submillimeter], Flux, Astrophysics, 01 natural sciences, Submillimeter Array, 0103 physical sciences, Radiative transfer, 010303 astronomy & astrophysics, Intergalactic medium, Line (formation), Physics, individual: cid_346 [quasars], 010308 nuclear & particles physics, Galaxies: high-redshift, Astronomy and Astrophysics, Quasar, Galaxies: active, Astrophysics - Astrophysics of Galaxies, Redshift, Submillimeter: galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Millimeter, intergalactic medium, Halo, Galaxies: halo, galaxies: active, quasars: individual: cid_346, galaxies: high-redshift, submillimeter: galaxies, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics, Quasars: individual: cid_346
Abstract: We present the discovery of copious molecular gas in the halo of cid_346, a $z=2.2$ quasar studied as part of the SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER). New Atacama Compact Array (ACA) CO(3-2) observations detect a much higher flux (by a factor of $14\pm5$) than measured on kiloparsec scales ($r\lesssim8$ kpc) using previous snapshot Atacama Large Millimeter/submillimeter Array data. Such additional CO(3-2) emission traces a structure that extends out to $r\sim200$ kpc in projected size, as inferred through direct imaging and confirmed by an analysis of the uv visibilities. This is the most extended molecular circumgalactic medium (CGM) reservoir that has ever been mapped. It shows complex kinematics, with an overall broad line profile (FWHM $= 1000$ km/s) that is skewed towards redshifted velocities up to at least $v\sim1000$ km/s. Using the optically thin assumption, we estimate a strict lower limit for the total molecular CGM mass observed by ACA of $M_{mol}^{CGM}>10^{10}~M_{\odot}$. There is however room for up to $M^{CGM}_{mol}\sim 1.7\times 10^{12}$ $M_{\odot}$, once optically thick CO emission with $\alpha_{\rm CO}=3.6$ $\rm M_{\odot}~(K~km~s^{-1}~pc^2)^{-1}$ and $L^{\prime}_{CO(3-2)}/L^{\prime}_{CO(1-0)}=0.5$ are assumed. Since cid_346 hosts quasar-driven ionised outflows and since there is no evidence of merging companions or an overdensity, we suggest that outflows may have played a crucial rule in seeding metal-enriched, dense gas on halo scales. However, the origin of such an extended molecular CGM remains unclear., Comment: Accepted for publication in A&A Letters. 9 pages and 9 figures including Appendix. Version updated after language editing
Published: 2021

43. Inquiring into the nature of the Abell 2667 Brightest Cluster Galaxy: physical properties from MUSE

Author: Pablo G. Pérez-González, Paolo Tozzi, A. Enia, Dario Fadda, G. Sabatini, G. Rodighiero, Giovanni Cresci, Joel Vernet, Piero Rosati, Amata Mercurio, Alberto Franceschini, S. Berta, G. B. Caminha, Jacopo Fritz, E. Iani, L. Morselli, R. J. van Weeren, A. Zanella, Chiara Mancini, L. Rodríguez-Muñoz, A. Liu, A. Concas, Paolo Cassata, P. Popesso, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Iani E., Rodighiero G., Fritz J., Cresci G., Mancini C., Tozzi P., Rodriguez-Munoz L., Rosati P., Caminha G.B., Zanella A., Berta S., Cassata P., Concas A., Enia A., Fadda D., Franceschini A., Liu A., Mercurio A., Morselli L., Perez-Gonzalez P.G., Popesso P., Sabatini G., Vernet J., Van Weeren R.J., and Astronomy
Subjects: ACTIVE GALACTIC NUCLEI, Astrofísica, Stellar kinematics, galaxies: clusters: intracluster medium, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, X-RAY SPECTROSCOPY, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, VELOCITY DISPERSION PROFILES, cD, STAR-FORMATION, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, galaxies: elliptical and lenticular, Brightest cluster galaxy, OPTICAL-SPECTRA, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, FAR-ULTRAVIOLET OBSERVATIONS, Physics, Supermassive black hole, 010308 nuclear & particles physics, Star formation, RICH CLUSTERS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: clusters: general, Space and Planetary Science, MOLECULAR-HYDROGEN, Astrophysics of Galaxies (astro-ph.GA), galaxies: elliptical and lenticular, cD, galaxies: evolution, COOLING FLOWS, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Based on HST and MUSE data, we probe the stellar and gas properties (i.e. kinematics, stellar mass, star formation rate) of the radio-loud brightest cluster galaxy (BCG) located at the centre of the X-ray luminous cool core cluster Abell 2667 (z = 0.2343). The bi-dimensional modelling of the BCG surface brightness profile reveals the presence of a complex system of substructures extending all around the galaxy. Clumps of different size and shape plunged into a more diffuse component constitute these substructures, whose intense 'blue' optical colour hints to the presence of a young stellar population. Our results depict the BCG as a massive (M_star ~ 1.38 x 10^11 M_sun) dispersion-supported spheroid (v_star < 150 km/s, sigma_0 ~ 216 km/s) hosting an active supermassive black hole (M_SMBH ~ 3.8 x 10^9 M_sun) whose optical features are typical of low ionisation nuclear emission line regions. Although the velocity pattern of the stars in the BCG is irregular, the stellar kinematics in the regions of the clumps show a positive velocity of ~ 100 km/s, similarly to the gas component. An analysis of the mechanism giving rise to the observed lines in the clumps through empirical diagnostic diagrams points out that the emission is composite, suggesting the contribution from both star formation and AGN. We conclude our analysis describing how scenarios of both chaotic cold accretion and merging with a gas-rich disc galaxy can efficaciously explain the phenomena the BCG is undergoing., Accepted for publication on the 10th of June 2019 (MNRAS)
Published: 2019
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44. Multi-phase outflows in Mkn 848 observed with SDSS-MaNGA integral field spectroscopy

Author: V. Mainieri, Filippo Mannucci, Alessandro Marconi, A. Concas, Giorgio Lanzuisi, Giovanni Cresci, Michele Perna, Marcella Brusa, ITA, GBR, DEU, and Perna M., Cresci G., Brusa M., Lanzuisi G., Concas A., Mainieri V., Mannucci F., Marconi A.
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Kinetic energy, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, galaxies: active, ISM: jets and outflows, galaxies: individual: Mkn 848, Astrophysics - Astrophysics of Galaxies, Momentum, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Ionization, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Field spectroscopy, Outflow, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The characterisation of galaxy-scale outflows in terms of their multi-phase nature, amount, and effects of flowing material is crucial to place constraints on models of galaxy evolution. This study can proceed only with the detailed investigation of individual targets. We present a spatially resolved spectroscopic optical data analysis of Mkn 848, a complex system consisting of two merging galaxies at z~0.04 that are separated 7.5 kpc (projected distance). Motivated by the presence of a multi-phase outflow in the north-west system revealed by the SDSS integrated spectrum, we analysed the publicly available MaNGA data, which cover almost the entire merging system, to study the physical properties of cool and warm gas in detail. Galaxy-wide outflowing gas in multiple phases is revealed for the first time in the two merging galaxies. We also detect spatially resolved resonant NaID emission associated with the outflows. The derived outflow energetics may be consistent with a scenario in which both winds are accelerated by stellar processes and AGN activity, although we favour an AGN origin given the high outflow velocities and the ionisation conditions observed in the outflow regions. Deeper observations are required, however, to better constrain the nature of these multi-phase outflows. Outflow energetics in the north-west system are strongly different between the ionised and atomic gas components, the latter of which is associated with mass outflow rate and kinetic and momentum powers that are 1-2 dex higher; those associated with the south-east galaxy are instead similar. Strong kp-scale outflows are revealed in an ongoing merger system, suggesting that feedback can potentially impact the host galaxy even in the early merger phases. The characterisation of the neutral and ionised gas phases has proved to be crucial for a comprehensive study of the outflow phenomena., Comment: 19 pages, 14 figures, accepted for publication in A&A
Published: 2019

45. The VANDELS survey: The relation between the UV continuum slope and stellar metallicity in star-forming galaxies at z ∼ 3

Author: M. Bolzonella, Fabio Fontanot, Nimish P. Hathi, Andrea Cimatti, P. Santini, Adriano Fontana, F. Mannucci, Laura Pentericci, G. Zamorani, Giovanni Cresci, Marco Castellano, A. Calabrò, A. Saxena, F. Marchi, M. Franco, Daniel Schaerer, Nicola Menci, Ricardo Amorín, Lizhi Xie, G. De Lucia, Johan P. U. Fynbo, Pascale Hibon, Margherita Talia, Ross J. McLure, Michaela Hirschmann, Fergus Cullen, Calabro A., Castellano M., Pentericci L., Fontanot F., Menci N., Cullen F., Mclure R., Bolzonella M., Cimatti A., Marchi F., Talia M., Amorin R., Cresci G., De Lucia G., Fynbo J., Fontana A., Franco M., Hathi N.P., Hibon P., Hirschmann M., Mannucci F., Santini P., Saxena A., Schaerer D., Xie L., and Zamorani G.
Subjects: Metallicity, Continuum (design consultancy), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), 01 natural sciences, abundances [galaxies], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, SPECTRAL-SYNTHESIS, FIELD, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, HIERARCHICAL FORMATION, 010308 nuclear & particles physics, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, GALACTIC STELLAR, stellar content [galaxies], Galaxies: stellar content, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Galaxy, TO 2, CHEMICAL ENRICHMENT, LYMAN-BREAK GALAXIES, ULTRAVIOLET LUMINOSITY DENSITY, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DUST OBSCURATION, Astrophysics::Earth and Planetary Astrophysics, high-redshift [galaxies], Galaxies: abundance
Abstract: The estimate of stellar metallicities (Z*) of high-z galaxies are of paramount importance in order to understand the complexity of dust effects and the reciprocal interrelations among stellar mass, dust attenuation, stellar age, and metallicity. Benefiting from uniquely deep FUV spectra of >500 star-forming galaxies at redshifts 2, Comment: 25 pages, 4 tables, 16 figures, and 5 Appendix subsections; accepted for publication in A&A
Published: 2021

46. A very dark stellar system lost in Virgo: kinematics and metallicity of SECCO 1 with MUSE

Author: Filippo Fraternali, Bernd Husemann, Michele Bellazzini, Lodovico Coccato, M. Correnti, Vincenzo Testa, Giovanni Cresci, S. Perina, Giuseppina Battaglia, Rodrigo A. Ibata, P. T. de Zeeuw, Laura Magrini, Giacomo Beccari, Nicolas F. Martin, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Astronomy, Beccari, G., Bellazzini, M., Magrini, L., Coccato, L., Cresci, G., Fraternali, F., de Zeeuw, P. T., Husemann, B., Ibata, R., Battaglia, G., Martin, N., Testa, V., Perina, S., and Correnti, M.
Subjects: Stellar kinematics, DWARF GALAXIES, 010504 meteorology & atmospheric sciences, Stellar mass, Metallicity, FOS: Physical sciences, POPULATION SYNTHESIS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, star formation, H-II REGIONS, H II regions, 0103 physical sciences, PHOTOMETRY, Astrophysics::Solar and Stellar Astrophysics, H II regions -galaxies, HIGH-VELOCITY CLOUDS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, Physics, Star formation, Local Group, Astronomy, CLUSTER, Astronomy and Astrophysics, galaxies: dwarf, Astrophysics - Astrophysics of Galaxies, Virgo Cluster, Galaxy, dwarf -galaxies, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, EVOLUTION DATABASE, Astrophysics::Earth and Planetary Astrophysics, H II regions – galaxies: dwarf – galaxies: star formation, HIGH-REDSHIFT, EMISSION, LOCAL GROUP
Abstract: We present the results of VLT-MUSE integral field spectroscopy of SECCO1, a faint, star-forming stellar system recently discovered as the stellar counterpart of an Ultra Compact High Velocity Cloud (HVC274.68+74.0), very likely residing within a substructure of the Virgo cluster of galaxies. We have obtained the radial velocity of a total of 38 individual compact sources identified as HII regions in the main and secondary body of the system, and derived the metallicity for 18 of them. We provide the first direct demonstration that the two stellar bodies of SECCO1 are physically associated and that their velocities match the HI velocities. The metallicity is quite uniform over the whole system, with a dispersion sigma_12+log(O/H/)=0.08, lower than the uncertainty on individual metallicity estimates. The mean abundance, 12+log(O/H)=8.44, is much higher than the typical values for local dwarf galaxies of similar stellar mass. This strongly suggests that the SECCO~1 stars were born from a pre-enriched gas cloud, possibly stripped from a larger galaxy. Using archival HST images we derive a total stellar mass of ~1.6 X 10^5 M_sun for SECCO1, confirming that it has a very high HI to stellar mass ratio for a dwarf galaxy, M_HI/M_*~ 100. The star formation rate, derived from the H_alpha flux is a factor of more than 10 higher than in typical dwarf galaxies of similar luminosity., Accepted for publication by MNRAS. pdfLaTeX. 10 pages, 4 figures, 4 tables
Published: 2016

47. Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

Author: V. Manieri, G. Zamorani, C. Vignali, F. Vito, Paolo Tozzi, Dimitra Rigopoulou, Francesca Pozzi, C. Norman, Roberto Gilli, Jacopo Fritz, Giovanni Cresci, Q. D'Amato, Anna Feltre, Viviana Casasola, Francesco Calura, C. Circosta, Marcella Massardi, D'Amato Q., Gilli R., Vignali C., Massardi M., Pozzi F., Zamorani G., Circosta C., Vito F., Fritz J., Cresci G., Casasola V., Calura F., Feltre A., Manieri V., Rigopoulou D., Tozzi P., and Norman C.
Subjects: Physics, Active galactic nucleus, 010308 nuclear & particles physics, Star formation, Astrophysics::High Energy Astrophysical Phenomena, ISM: structure, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: active, Astrophysics, 01 natural sciences, Submillimeter Array, Redshift, Galaxy, Interstellar medium, Submillimeter: galaxies, Space and Planetary Science, ISM: kinematics and dynamic, 0103 physical sciences, Chandra Deep Field South, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. Obscured active galactic nuclei (AGN) represent a significant fraction of the entire AGN population, especially at high redshift (∼70% at z = 3 − 5). They are often characterized by the presence of large gas and dust reservoirs that are thought to sustain and possibly obscure vigorous star formation processes that make these objects shine at FIR and submillimeter wavelengths. Studying the physical properties of obscured AGN and their host galaxies is crucial to shedding light on the early stages of a massive system lifetime. Aims. We aim to investigate the contribution of the interstellar medium (ISM) to the obscuration of quasars in a sample of distant highly star forming galaxies and to unveil their morphological and kinematics properties. Methods. We exploit Atacama Large Millimeter/submillimeter Array Cycle 4 observations of the continuum (∼2.1 mm) and high-J CO emission of a sample of six X-ray selected, FIR detected galaxies hosting an obscured AGN at zspec > 2.5 in the 7 Ms Chandra Deep Field-South. We measured the masses and sizes of the dust and molecular gas by fitting the images, visibilities, and spectra, and we derived the gas density and column density on the basis of a uniform sphere geometry. Finally, we compared the measured column densities with those derived from the Chandra X-ray spectra. Results. We detected both the continuum and line emission for three sources for which we measured both the flux density and size. For the undetected sources, we derived an upper limit on the flux density from the root mean square of the images. We found that the detected galaxies are rich in gas and dust (molecular gas mass in the range < 0.5–2.7 × 1010 M⊙ for αCO = 0.8 and up to ∼2 × 1011 M⊙ for αCO = 6.5, and dust mass < 0.9–4.9 × 108 M⊙) and generally compact (gas major axis 2.1–3.0 kpc, dust major axis 1.4–2.7 kpc). The column densities associated with the ISM are on the order of 1023 − 24 cm−2, which is comparable with those derived from the X-ray spectra. For the detected sources we also derived dynamical masses in the range 0.8–3.7 × 1010 M⊙. Conclusions. We conclude that the ISM of high redshift galaxies can substantially contribute to nuclear obscuration up to the Compton-thick (> 1024 cm−2) regime. In addition, we found that all the detected sources show a velocity gradient reminding one rotating system, even though two of them show peculiar features in their morphology that can be associated with a chaotic, possibly merging, structure.
Published: 2020

48. The VANDELS ESO public spectroscopic survey

Author: H. Mendez-Hernandez, Matt J. Jarvis, Mark Dickinson, D. Maccagni, Lucia Pozzetti, Ricardo Amorín, Christina C. Williams, B. Garilli, Eros Vanzella, David T. Maltby, A. Iovino, Omar Almaini, Marco Castellano, Antonis Georgakakis, Italo Balestra, Daniel Schaerer, M. Mignoli, Y. Khusanova, D. P. Rosario, Steve Finkelstein, P. Popesso, Andrea Grazian, Marcella Brusa, Anton M. Koekemoer, Maurilio Pannella, S. Juneau, Ross J. McLure, Michele Cirasuolo, Vivienne Wild, P. Santini, Nimish P. Hathi, K. Matsuoka, Seock-Sam Kim, Giovanni Cresci, Kirpal Nandra, Jairo Méndez-Abreu, Fabio Fontanot, F. Mannucci, A. C. Carnall, Laura Pentericci, Eric F. Bell, P. Franzetti, Fernando Buitrago, Michele Moresco, D. J. McLeod, Andrea Cimatti, Adriana Gargiulo, James Dunlop, E. Curtis-Lake, Rebecca A. A. Bowler, S. de Barros, Fabrizio Fiore, M. Bolzonella, D. Elbaz, Johan P. U. Fynbo, Giovanni G. Fazio, Margherita Talia, V. Sommariva, Marco Scodeggio, Stefano Cristiani, Jennifer M. Lotz, S. Bardelli, Mario Nonino, M. Giavalisco, Corentin Schreiber, Mara Salvato, Henry C. Ferguson, Audrey Galametz, E. Zucca, O. Le Fevre, Angela Bongiorno, M. Fumana, L. A. M. Tasca, Daniel P. Stark, Nathan Bourne, F. Marchi, M. Franco, W. G. Hartley, Stéphane Charlot, Adriano Fontana, Paolo Cassata, E. Mármol-Queraltó, W. Karman, Karina Caputi, Tommaso Treu, R. Thomas, Casey Papovich, Emanuela Pompei, O. Cucciati, Alice Mortlock, Annalisa Citro, Fergus Cullen, Intae Jung, G. Zamorani, Lucia Guaita, Astronomy, McLure, R. J., Pentericci, L., Cimatti, A., Dunlop, J. S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S. L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W. G., Iovino, A., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Mármol-Queraltó, E., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), Department of Surgery, Santi Giovanni e Paolo Hospital, Association de Coordination Technique Agricole (ACTA), Space Telescope Science Institute (STSci), 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), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Department of Agronomy, Food, Natural Resources, Animals and the Environment (DAFNAE), Universita degli Studi di Padova, Institute for General Botany, Johannes Gutenberg - Universität Mainz (JGU), Les instituts techniques agricoles (Acta), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository
Subjects: Active galactic nucleus, Stellar population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Survey, 010303 astronomy & astrophysics, Galaxies: high, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Galaxies: evolution, Galaxies: star formation, Surveys, Chandra Deep Field South, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract: VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO's Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < lambda < 1.0 micron) spectroscopy of ~2100 galaxies within the redshift interval 1.0 < z < 7.0, over a total area of ~0.2 sq. degrees centred on the CANDELS UDS and CDFS fields. Based on accurate photometric redshift pre-selection, 85% of the galaxies targeted by VANDELS were selected to be at z>=3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < t_int < 80 hours), the VANDELS survey targeted: a) bright star-forming galaxies at 2.4 < z < 5.5, b) massive quiescent galaxies at 1.0 < z < 2.5, c) fainter star-forming galaxies at 3.0 < z < 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design and target selection., 19 pages, 9 figures, accepted for publication in MNRAS
Published: 2018

49. The VANDELS ESO public spectroscopic survey: observations and first data release

Author: O. Cucciati, Andrea Grazian, E. Zucca, Y. Khusanova, Emma Curtis-Lake, A. Iovino, Stéphane Charlot, R. J. McLure B. Garilli, James Dunlop, Adriana Gargiulo, Johan P. U. Fynbo, Alice Mortlock, Mara Salvato, E. Mármol-Queraltó, Nimish P. Hathi, Seock-Sam Kim, L. A. M. Tasca, Fabrizio Fiore, Italo Balestra, Kirpal Nandra, A. Georgakakis, Emanuela Pompei, D. Elbaz, Anton M. Koekemoer, S. L. Finkelstein, F. Marchi, M. Franco, Maurilio Pannella, Tommaso Treu, Audrey Galametz, Corentin Schreiber, H. Mendez-Hernandez, Andrea Cimatti, P. Popesso, M. Fumana, Giovanni G. Fazio, S. Cristiani, Angela Bongiorno, David J. Rosario, Laura Pentericci, Marco Castellano, Piero Rosati, Vivienne Wild, Giovanni Cresci, A. C. Carnall, C. Caputi, M. Giavalisco, Paolo Cassata, Lucia Pozzetti, Marcella Brusa, M. Bolzonella, R. C. Thomas, Margherita Talia, D. Maccagni, S. Bardelli, W. Karman, S. DeBarros, K. Matsuoka, H. C. Ferguson, Jennifer M. Lotz, F. Fontanot, Adriano Fontana, C. Papovich, W. G. Hartley, Michele Moresco, Eros Vanzella, David T. Maltby, Omar Almaini, S. Juneau, Rebecca A. A. Bowler, Daniel Schaerer, Daniel P. Stark, Nathan Bourne, S. M. Faber, D. J. McLeod, Ricardo Amorín, Michele Cirasuolo, P. Franzetti, Fernando Buitrago, O. Le Fevre, Annalisa Citro, Mario Nonino, Fergus Cullen, Intae Jung, G. Zamorani, Eric F. Bell, Lucia Guaita, Christina C. Williams, V. Sommariva, Marco Scodeggio, M. Mignoli, Matt J. Jarvis, Mark Dickinson, P. Santini, Jairo Méndez-Abreu, F. Mannucci, ITA, USA, GBR, FRA, DEU, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Milano (OAM), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Brera (OAB), Università di Bologna, Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), INAF - Osservatorio Astronomico di Bologna (OAB), 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), CNR-INFM CRS-Soft, c/o Dipartimento di Fisica, CNR-INFM CRS-Soft, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), INAF-IASF Milano, European Southern Observatory (ESO), University of Bologna, INAF - Osservatorio Astronomico di Trieste (OAT), Dipartimento di Fisica e Astronomia [Bologna], University of Groningen [Groningen], Laboratoire d'Astrophysique de Marseille (LAM), 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), Osservatorio Astronomico (INAF), NOAO, Max-Planck-Institut für Extraterrestrische Physik (MPE), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Space Telescope Science Institute (STSci), Department of computer science, Kyushu Institute of Technology, University of Texas-Pan American (UTPA), University of Texas-Pan, Excellence Cluster Universe, Technische Universität München [München] (TUM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), National Optical Astronomy Observatory (NOAO), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, 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), University of Bologna/Università di Bologna, 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), Kyushu Institute of Technology (Kyutech), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Pentericci, L., McLure, R. J., Garilli, B., Cucciati, O., Franzetti, P., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., De Barros, S., Dunlop, J. S., Elbaz, D., Finkelstein, S. L., Fontana, A., Fontanot, F., Fumana, M., Gargiulo, A., Guaita, L., Hartley, W. G., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Marmol-Queralto, E., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository
Subjects: media_common.quotation_subject, REDSHIFT, Galaxies: fundamental parameter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, fundamental parameters [galaxies], QB Astronomy, Survey, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: general, Galaxies: high-redshift, Surveys, Astronomy and Astrophysics, Space and Planetary Science, 010303 astronomy & astrophysics, Spectrograph, evolution [galaxies], QC, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, media_common, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, galaxies: fundamental parameters, 3rd-DAS, Astronomy and Astrophysic, galaxies: general, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Universe, Data set, GALAXIES, QC Physics, Sky, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), VIMOS, galaxies: evolution, high-redshift [galaxies], Data reduction, general [galaxies]
Abstract: This paper describes the observations and the first data release (DR1) of the ESO public spectroscopic survey "VANDELS, a deep VIMOS survey of the CANDELS CDFS and UDS fields". VANDELS' main targets are star-forming galaxies at 2.4, Comment: Submitted to A&A
Published: 2018

50. Ionized Gas Outflows from the MAGNUM Survey: NGC 1365 and NGC 4945

Author: Giacomo Venturi, Alessandro Marconi, Matilde Mingozzi, Stefano Carniani, Giovanni Cresci, Guido Risaliti, Filippo Mannucci, Venturi, G., Marconi, A., Mingozzi, M., Carniani, S., Cresci, G., Risaliti, G., and Mannucci, F.
Subjects: Active galactic nucleus, lcsh:Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, imaging spectroscopy, 01 natural sciences, outflows, lcsh:QB1-991, Integral field spectrograph, NGC 4945, Settore FIS/05 - Astronomia e Astrofisica, galaxies, 0103 physical sciences, Radiative transfer, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, galaxie, lcsh:QC801-809, Astronomy and Astrophysics, Quasar, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, lcsh:Geophysics. Cosmic physics, NGC 1365, Astrophysics of Galaxies (astro-ph.GA), active galactic nuclei, Outflow, Galaxies, Outflows
Abstract: AGN feedback, acting through strong outflows accelerated in the nuclear region of AGN hosts, is invoked as a key ingredient for galaxy evolution by many models to explain the observed BH-galaxy scaling relations. Recently, some direct observational evidence of radiative mode feedback in action has been finally found in quasars at $z$>1.5. However, it is not possible to study outflows in quasars at those redshifts on small scales ($\lesssim$100 pc), as spatial information is limited by angular resolution. This is instead feasible in nearby active galaxies, which are ideal laboratories to explore outflow structure and properties, as well as the effects of AGN on their host galaxies. In this proceeding we present preliminary results from the MAGNUM survey, which comprises nearby Seyfert galaxies observed with the integral field spectrograph VLT/MUSE. We focus on two sources, NGC 1365 and NGC 4945, that exhibit double conical outflows extending on distances >1 kpc. We disentangle the dominant contributions to ionization of the various gas components observed in the central $\sim$5.3 kpc of NGC 1365. An attempt to infer outflow 3D structure in NGC 4945 is made via simple kinematic modeling, suggesting a hollow cone geometry., 9 pages, 2 figures. This proceeding is part of the Research Topic "Quasars at all cosmic epochs", following the conference in Padova, Italy, on April 2-7, 2017
Published: 2018
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