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282 results on '"Sargent M. T."'

51. GOODS-ALMA 2.0: Starbursts in the main sequence reveal compact star formation regulating galaxy evolution prequenching

Author

Gómez-Guijarro, C., primary, Elbaz, D., additional, Xiao, M., additional, Kokorev, V. I., additional, Magdis, G. E., additional, Magnelli, B., additional, Daddi, E., additional, Valentino, F., additional, Sargent, M. T., additional, Dickinson, M., additional, Béthermin, M., additional, Franco, M., additional, Pope, A., additional, Kalita, B. S., additional, Ciesla, L., additional, Demarco, R., additional, Inami, H., additional, Rujopakarn, W., additional, Shu, X., additional, Wang, T., additional, Zhou, L., additional, Alexander, D. M., additional, Bournaud, F., additional, Chary, R., additional, Ferguson, H. C., additional, Finkelstein, S. L., additional, Giavalisco, M., additional, Iono, D., additional, Juneau, S., additional, Kartaltepe, J. S., additional, Lagache, G., additional, Le Floc’h, E., additional, Leiton, R., additional, Leroy, L., additional, Lin, L., additional, Motohara, K., additional, Mullaney, J., additional, Okumura, K., additional, Pannella, M., additional, Papovich, C., additional, and Treister, E., additional

Published
2022
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52. A model for the infrared-radio correlation of main-sequence galaxies at GHz frequencies and its dependence on redshift and stellar mass

Author

Schober, J., Sargent, M. T., Klessen, R. S., and Schleicher, D. R. G.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

The infrared-radio correlation (IRRC) of star-forming galaxies can be used to estimate their star formation rate (SFR) based on the radio continuum luminosity at MHz-GHz frequencies. For application in future deep radio surveys, it is crucial to know whether the IRRC persists at high redshift z. Delvecchio et al. (2020) observed that the 1.4 GHz IRRC correlation of star-forming galaxies is nearly z-invariant up to z~4, but depends strongly on the stellar mass M_star. This should be taken into account for SFR calibrations based on radio luminosity. To understand the physical cause of the M_star-dependence of the IRRC and its properties at higher z, we construct a phenomenological model for galactic radio emission involving magnetic fields generated by a small-scale dynamo, a steady-state cosmic ray population, as well as observed scaling relations that reduce the number of free parameters. The best agreement between the model and the characteristics of the IRRC observed by Delvecchio et al. (2020) is found when the efficiency of the SN-driven turbulence is 5 % and when saturation of the small-scale dynamo occurs once 10 % of the kinetic energy is converted into magnetic energy. The observed dependence of the IRRC on M_star and z can be reproduced with our model. For galaxies with intermediate to high (M_star ~ 10^9.5 - 10^11 M_sun) stellar masses, our model results in a IRRC which is nearly independent of z. For galaxies with lower masses (M_star ~ 10^8.5 M_sun), we find that the IR-to-radio flux ratio increases with increasing redshift. This matches the observational data in that mass bin which, however, only extends to z~1.5. The increase of the IR-to-radio flux ratio for low-mass galaxies at z>1.5 that is predicted by our model could be tested with future deep radio observations., 20 pages, 18 figures, submitted to A&A

Published
2022
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53. The hidden side of cosmic star formation at z >3: Bridging optically dark and Lyman-break galaxies with GOODS-ALMA.

Author

Xiao, M.-Y., Elbaz, D., Gómez-Guijarro, C., Leroy, L., Bing, L.-J., Daddi, E., Magnelli, B., Franco, M., Zhou, L., Dickinson, M., Wang, T., Rujopakarn, W., Magdis, G. E., Treister, E., Inami, H., Demarco, R., Sargent, M. T., Shu, X., Kartaltepe, J. S., and Alexander, D. M.

Subjects
STAR formation, GALAXIES, DISTRIBUTION of stars, STELLAR mass, GALACTIC redshift, GAUSSIAN measures
Abstract

Our current understanding of the cosmic star formation history at z > 3 is primarily based on UV-selected galaxies (Lyman-break galaxies, i.e., LBGs). Recent studies of H-dropouts (HST-dark galaxies) have revealed that we may be missing a large proportion of star formation that is taking place in massive galaxies at z > 3. In this work, we extend the H-dropout criterion to lower masses to select optically dark or faint galaxies (OFGs) at high redshifts in order to complete the census between LBGs and H-dropouts. Our criterion (H > 26:5 mag & [4.5] < 25 mag) combined with a de-blending technique is designed to select not only extremely dust-obscured massive galaxies but also normal star-forming galaxies (typically E(B V) > 0:4) with lower stellar masses at high redshifts. In addition, with this criterion, our sample is not contaminated by massive passive or old galaxies. In total, we identified 27 OFGs at zphot > 3 (with a median of zmed = 4:1) in the GOODS-ALMA field, covering a wide distribution of stellar masses with log(MM) = 9:411:1 (with a median of log(Med/M) = 10.3). We find that up to 75% of the OFGs with log(M/M) = 9:510:5 were neglected by previous LBGs and H-dropout selection techniques. After performing an optical-to-millimeter stacking analysis of the OFGs, we find that rather than being limited to a rare population of extreme starbursts, these OFGs represent a normal population of dusty star-forming galaxies at z > 3. The OFGs exhibit shorter gas depletion timescales, slightly lower gas fractions, and lower dust temperatures than the scaling relation of typical star-forming galaxies. Additionally, the total star formation rate (SFRtot = SFRIR + SFRUV) of the stacked OFGs is much higher than the SFRcorr UV (SFRUV corrected for dust extinction), with an average SFRtot/SFRcorr UV = 8 ± 1, which lies above (~0.3 dex) the 16-84th percentile range of typical star-forming galaxies at 3 z 6. All of the above suggests the presence of hidden dust regions in the OFGs that absorb all UV photons, which cannot be reproduced with dust extinction corrections. The effective radius of the average dust size measured by a circular Gaussian model fit in the uv plane is Re(1:13 mm) = 1:01 ± 0:05 kpc. After excluding the five LBGs in the OFG sample, we investigated their contributions to the cosmic star formation rate density (SFRD). We found that the SFRD at z > 3 contributed by massive OFGs (log(MM) > 10:3) is at least two orders of magnitude higher than the one contributed by equivalently massive LBGs. Finally, we calculated the combined contribution of OFGs and LBGs to the cosmic SFRD at z = 45 to be 4 102 M yr1 Mpc3, which is about 0.15 dex (43%) higher than the SFRD derived from UV-selected samples alone at the same redshift. This value could be even larger, as our calculations were performed in a very conservative way. [ABSTRACT FROM AUTHOR]

Published
2023
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54. GOODS-ALMA 2.0: Source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies

Author

Gómez-Guijarro, C., primary, Elbaz, D., additional, Xiao, M., additional, Béthermin, M., additional, Franco, M., additional, Magnelli, B., additional, Daddi, E., additional, Dickinson, M., additional, Demarco, R., additional, Inami, H., additional, Rujopakarn, W., additional, Magdis, G. E., additional, Shu, X., additional, Chary, R., additional, Zhou, L., additional, Alexander, D. M., additional, Bournaud, F., additional, Ciesla, L., additional, Ferguson, H. C., additional, Finkelstein, S. L., additional, Giavalisco, M., additional, Iono, D., additional, Juneau, S., additional, Kartaltepe, J. S., additional, Lagache, G., additional, Le Floc’h, E., additional, Leiton, R., additional, Lin, L., additional, Motohara, K., additional, Mullaney, J., additional, Okumura, K., additional, Pannella, M., additional, Papovich, C., additional, Pope, A., additional, Sargent, M. T., additional, Silverman, J. D., additional, Treister, E., additional, and Wang, T., additional

Published
2022
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55. FR-type radio sources at 3 GHz VLA-COSMOS: Relation to physical properties and large-scale environment

Author

Vardoulaki, E., primary, Jiménez Andrade, E. F., additional, Delvecchio, I., additional, Smolčić, V., additional, Schinnerer, E., additional, Sargent, M. T., additional, Gozaliasl, G., additional, Finoguenov, A., additional, Bondi, M., additional, Zamorani, G., additional, Badescu, T., additional, Leslie, S. K., additional, Ceraj, L., additional, Tisanić, K., additional, Karim, A., additional, Magnelli, B., additional, Bertoldi, F., additional, Romano-Diaz, E., additional, and Harrington, K., additional

Published
2021
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56. The infrared-radio correlation of star-forming galaxies is stronglyM⋆-dependent but nearly redshift-invariant sincez∼ 4

Author

Delvecchio, I., primary, Daddi, E., additional, Sargent, M. T., additional, Jarvis, M. J., additional, Elbaz, D., additional, Jin, S., additional, Liu, D., additional, Whittam, I. H., additional, Algera, H., additional, Carraro, R., additional, D’Eugenio, C., additional, Delhaize, J., additional, Kalita, B. S., additional, Leslie, S., additional, Molnár, D. Cs., additional, Novak, M., additional, Prandoni, I., additional, Smolčić, V., additional, Ao, Y., additional, Aravena, M., additional, Bournaud, F., additional, Collier, J. D., additional, Randriamampandry, S. M., additional, Randriamanakoto, Z., additional, Rodighiero, G., additional, Schober, J., additional, White, S. V., additional, and Zamorani, G., additional

Published
2021
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58. The e-MERGE Survey (e-MERLIN Galaxy Evolution Survey): overview and survey description

Author

Muxlow, T W B, primary, Thomson, A P, additional, Radcliffe, J F, additional, Wrigley, N H, additional, Beswick, R J, additional, Smail, Ian, additional, McHardy, I M, additional, Garrington, S T, additional, Ivison, R J, additional, Jarvis, M J, additional, Prandoni, I, additional, Bondi, M, additional, Guidetti, D, additional, Argo, M K, additional, Bacon, David, additional, Best, P N, additional, Biggs, A D, additional, Chapman, S C, additional, Coppin, K, additional, Chen, H, additional, Garratt, T K, additional, Garrett, M A, additional, Ibar, E, additional, Kneib, Jean-Paul, additional, Knudsen, Kirsten K, additional, Koopmans, L V E, additional, Morabito, L K, additional, Murphy, E J, additional, Njeri, A, additional, Pearson, Chris, additional, Pérez-Torres, M A, additional, Richards, A M S, additional, Röttgering, H J A, additional, Sargent, M T, additional, Serjeant, Stephen, additional, Simpson, C, additional, Simpson, J M, additional, Swinbank, A M, additional, Varenius, E, additional, and Venturi, T, additional

Published
2020
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60. A hyper luminous starburst at z = 4.72 magnified by a lensing galaxy pair at z = 1.48

Author

Ciesla, L., primary, Béthermin, M., additional, Daddi, E., additional, Richard, J., additional, Diaz-Santos, T., additional, Sargent, M. T., additional, Elbaz, D., additional, Boquien, M., additional, Wang, T., additional, Schreiber, C., additional, Yang, C., additional, Zabl, J., additional, Fraser, M., additional, Aravena, M., additional, Assef, R. J., additional, Baker, A. J., additional, Beelen, A., additional, Boselli, A., additional, Bournaud, F., additional, Burgarella, D., additional, Charmandaris, V., additional, Côté, P., additional, Epinat, B., additional, Ferrarese, L., additional, Gobat, R., additional, and Ilbert, O., additional

Published
2020
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61. The e-MERGE Survey (e-MERLIN Galaxy Evolution Survey): overview and survey description

Author

Muxlow, T W B, Thomson, A P, Radcliffe, J F, Wrigley, N H, Beswick, R J, Smail, Ian, McHardy, I M, Garrington, S T, Ivison, R J, Jarvis, M J, Prandoni, I, Bondi, M, Guidetti, D, Argo, Megan, Bacon, David, Best, P N, Biggs, A D, Chapman, S C, Coppin, K, Chen, H, Garratt, T K, Garrett, M A, Ibar, E, Kneib, Jean-Paul, Knudsen, Kirsten K, Koopmans, L V E, Morabito, L K, Murphy, E J, Njeri, A, Pearson, Chris, Pérez-Torres, M A, Richards, A M S, Röttgering, H J A, Sargent, M T, Serjeant, Stephen, Simpson, C, Simpson, J M, Swinbank, A M, Varenius, E, Venturi, T, Muxlow, T W B, Thomson, A P, Radcliffe, J F, Wrigley, N H, Beswick, R J, Smail, Ian, McHardy, I M, Garrington, S T, Ivison, R J, Jarvis, M J, Prandoni, I, Bondi, M, Guidetti, D, Argo, Megan, Bacon, David, Best, P N, Biggs, A D, Chapman, S C, Coppin, K, Chen, H, Garratt, T K, Garrett, M A, Ibar, E, Kneib, Jean-Paul, Knudsen, Kirsten K, Koopmans, L V E, Morabito, L K, Murphy, E J, Njeri, A, Pearson, Chris, Pérez-Torres, M A, Richards, A M S, Röttgering, H J A, Sargent, M T, Serjeant, Stephen, Simpson, C, Simpson, J M, Swinbank, A M, Varenius, E, and Venturi, T

Abstract

We present an overview and description of the e-MERGE Survey (e-MERLIN Galaxy Evolution Survey) Data Release 1 (DR1), a large program of high-resolution 1.5-GHz radio observations of the GOODS-N field comprising ∼140 h of observations with enhanced-Multi-Element Remotely Linked Interferometer Network (e-MERLIN) and ∼40 h with the Very Large Array (VLA). We combine the long baselines of e-MERLIN (providing high angular resolution) with the relatively closely packed antennas of the VLA (providing excellent surface brightness sensitivity) to produce a deep 1.5-GHz radio survey with the sensitivity (${\sim}1.5\, \mu$ Jy beam−1), angular resolution (0.2–0.7 arcsec) and field-of-view (∼15 × 15 arcmin2) to detect and spatially resolve star-forming galaxies and active galactic nucleus (AGN) at $z$ ≳ 1. The goal of e-MERGE is to provide new constraints on the deep, sub-arcsecond radio sky which will be surveyed by SKA1-mid. In this initial publication, we discuss our data analysis techniques, including steps taken to model in-beam source variability over an ∼20-yr baseline and the development of new point spread function/primary beam models to seamlessly merge e-MERLIN and VLA data in the uv plane. We present early science results, including measurements of the luminosities and/or linear sizes of ∼500 galaxies selected at 1.5 GHz. In combination with deep Hubble Space Telescope observations, we measure a mean radio-to-optical size ratio of re-MERGE/rHST ∼ 1.02 ± 0.03, suggesting that in most high-redshift galaxies, the ∼GHz continuum emission traces the stellar light seen in optical imaging. This is the first in a series of papers that will explore the ∼kpc-scale radio properties of star-forming galaxies and AGN in the GOODS-N field observed by e-MERGE DR1.

Published
2020

62. A3COSMOS:the dust attenuation of star-forming galaxies at z=2.5-4.0 from the COSMOS-ALMA archive

Author

Fudamoto, Yoshinobu, Oesch, P. A., Magnelli, B., Schinnerer, E., Liu, D., Lang, P., Jimenez-Andrade, E. E., Groves, B., Leslie, S., Sargent, M. T., Fudamoto, Yoshinobu, Oesch, P. A., Magnelli, B., Schinnerer, E., Liu, D., Lang, P., Jimenez-Andrade, E. E., Groves, B., Leslie, S., and Sargent, M. T.

Abstract

We present an analysis of the dust attenuation of star-forming galaxies at z = 2.5-4.0 through the relationship between the UV spectral slope (beta), stellar mass (M-*), and the infrared excess (IRX = L-IR/L-UV) based on far-infrared continuum observations from the Atacama Large Millimeter/sub-millimeter Array (ALMA). Our study exploits the full ALMA archive over the COSMOS field processed by the A3COSMOS team, which includes an unprecedented sample of similar to 1500 galaxies at z similar to 3 as primary or secondary targets in ALMA band 6 or 7 observations with a median continuum sensitivity of 126 mu Jy beam(-1) (1 sigma). The detection rate is highly mass dependent, decreasing drastically below log (M-*/M-circle dot) = 10.5. The detected galaxies show that the IRX-beta relationship of massive (logM(*)/M-circle dot > 10) main-sequence galaxies at z = 2.5-4.0 is consistent with that of local galaxies, while starbursts are generally offset by similar to 0.5 dex to larger IRX values. At the low-mass end, we derive upper limits on the infrared luminosities through stacking of the ALMA data. The combined IRX-M-* relation at log (M-*/M-circle dot) > 9 exhibits a significantly steeper slope than reported in previous studies at similar redshifts, implying little dust obscuration at logM(*)/M-circle dot <10. However, our results are consistent with earlier measurements at z similar to 5.5, indicating a potential redshift evolution between z similar to 2 and z similar to 6. Deeper observations targeting low-mass galaxies will be required to confirm this finding.

Published
2020

64. A closer look at the deep radio sky: Multi-component radio sources at 3 GHz VLA-COSMOS

Author

Vardoulaki, E., primary, Jiménez Andrade, E. F., additional, Karim, A., additional, Novak, M., additional, Leslie, S. K., additional, Tisanić, K., additional, Smolčić, V., additional, Schinnerer, E., additional, Sargent, M. T., additional, Bondi, M., additional, Zamorani, G., additional, Magnelli, B., additional, Bertoldi, F., additional, Herrera Ruiz, N., additional, Mooley, K. P., additional, Delhaize, J., additional, Myers, S. T., additional, Marchesi, S., additional, Koekemoer, A. M., additional, Gozaliasl, G., additional, Finoguenov, A., additional, Middleberg, E., additional, and Ciliegi, P., additional

Published
2019
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67. Automated Mining of the ALMA Archive in the COSMOS Field (A3COSMOS). II. Cold Molecular Gas Evolution out to Redshift 6

Author

Liu, Daizhong, Schinnerer, Eva, Groves, Brent, Magnelli, B, Lang, Philipp, Leslie, S K, Jiménez-Andrade, E., Riechers, Dominik, Popping, Gergo, Magdis, Georgios E, Daddi, E, Sargent, M T, Gao, Yu, Liu, Daizhong, Schinnerer, Eva, Groves, Brent, Magnelli, B, Lang, Philipp, Leslie, S K, Jiménez-Andrade, E., Riechers, Dominik, Popping, Gergo, Magdis, Georgios E, Daddi, E, Sargent, M T, and Gao, Yu

Abstract

We present new measurements of the cosmic cold molecular gas evolution out to redshift 6 based on systematic mining of the Atacama Large Millimeter/submillimeter Array (ALMA) public archive in the COSMOS deep field (A3COSMOS). Our A3COSMOS data set contains ~700 galaxies (0.3 lesssim z lesssim 6) with high-confidence ALMA detections in the (sub)millimeter continuum and multiwavelength spectral energy distributions. Multiple gas mass calibration methods are compared, and biases in band conversions (from observed ALMA wavelength to rest-frame Rayleigh-Jeans tail continuum) have been tested. Combining our A3COSMOS sample with ~1000 CO-observed galaxies at 0 lesssim z lesssim 4 (75% at z < 0.1), we parameterize galaxies' molecular gas depletion time (${\tau }_{\mathrm{depl}}$) and molecular gas to stellar mass ratio (${\mu }_{\mathrm{molgas}}$) each as a function of the stellar mass (${M}_{\star }$), offset from the star-forming main sequence (${\rm{\Delta }}\mathrm{MS}$) and cosmic age (or redshift). Our proposed functional form provides a statistically better fit to current data (than functional forms in the literature) and implies a "downsizing" effect (i.e., more-massive galaxies evolve earlier than less-massive ones) and "mass quenching" (gas consumption slows down with cosmic time for massive galaxies but speeds up for low-mass ones). Adopting galaxy stellar mass functions and applying our ${\mu }_{\mathrm{molgas}}$ function for gas mass calculation, we for the first time infer the cosmic cold molecular gas density evolution out to redshift 6 and find agreement with CO blind surveys as well as semianalytic modeling. These together provide a coherent picture of cold molecular gas, star formation rate, and stellar mass evolution in galaxies across cosmic time.

Published
2019

68. Radio Continuum Emission from Galaxies: An Accounting of Energetic Processes

Author

Murphy, E.J., Condon, J. J., Alberdi, Antxón, Barcos-Muñozarcos, L., Beswick, R. J., Brinks, E., Dong, D., Evans, A. S., Johnson, K. E., Kennicutt, R. C., Jr., Linden, S. T., Muxlow, T. W. B., Pérez-Torres, Miguel A., Schinnerer, E., Sargent, M. T., Tabatabaei, F. S., and Turner, J. L.

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, health care economics and organizations, Astrophysics::Galaxy Astrophysics
Abstract

Science with a Next Generation Very Large Array, ASP Conference Series, Vol. 517. ASP Monograph 7, Radio continuum observations have proven to be a workhorse in our understanding of the star formation process (i.e., stellar birth and death) from galaxies both in the nearby universe and out to the highest redshifts. In this article we focus on how the ngVLA will transform our understanding of star formation by enabling one to map and decompose the radio continuum emission from large, heterogeneous samples of nearby galaxies on greater than or similar to 10 pc scales to conduct a proper accounting of the energetic processes powering it. At the discussed sensitivity and angular resolution, the ngVLA will simultaneously be able to create maps of current star formation activity at similar to 100 pc scales, as well as detect and characterize (e.g., size, spectral shape, density, etc.) discrete Hn regions and supernova remnants on 10 pc scales in galaxies out to the distance of the Virgo cluster. Their properties can then be used to see how they relate to the local and global ISM and star formation conditions. Such investigations are essential for understanding the astrophysics of high-z measurements of galaxies, allowing for proper modeling of galaxy formation and evolution. © Copyright 2018 - Astronomical Society of the Pacific

Published
2018

69. A3COSMOS: the dust attenuation of star-forming galaxies at z = 2.5–4.0 from the COSMOS-ALMA archive.

Author

Fudamoto, Yoshinobu, Oesch, P A, Magnelli, B, Schinnerer, E, Liu, D, Lang, P, Jiménez-Andrade, E F, Groves, B, Leslie, S, and Sargent, M T

Subjects
DUST, STELLAR mass, STARBURSTS, GALAXIES, GALACTIC evolution, GALAXY formation
Abstract

We present an analysis of the dust attenuation of star-forming galaxies at z  = 2.5–4.0 through the relationship between the UV spectral slope (β), stellar mass (M *), and the infrared excess (IRX = L IR/ L UV) based on far-infrared continuum observations from the Atacama Large Millimeter/sub-millimeter Array (ALMA). Our study exploits the full ALMA archive over the COSMOS field processed by the A3COSMOS team, which includes an unprecedented sample of ∼1500 galaxies at z ∼ 3 as primary or secondary targets in ALMA band 6 or 7 observations with a median continuum sensitivity of 126 |$\rm {\mu Jy\, beam}^{-1}$| (1σ). The detection rate is highly mass dependent, decreasing drastically below log (M */M⊙) = 10.5. The detected galaxies show that the IRX–β relationship of massive (log  M */M⊙ > 10) main-sequence galaxies at z  = 2.5–4.0 is consistent with that of local galaxies, while starbursts are generally offset by |$\sim 0.5\, {\rm dex}$| to larger IRX values. At the low-mass end, we derive upper limits on the infrared luminosities through stacking of the ALMA data. The combined IRX– M * relation at |$\rm {log\, ({\it M}_{\ast }/\mathrm{M}_{\odot })\gt 9}$| exhibits a significantly steeper slope than reported in previous studies at similar redshifts, implying little dust obscuration at log  M */M⊙ < 10. However, our results are consistent with earlier measurements at z ∼ 5.5, indicating a potential redshift evolution between z ∼ 2 and z ∼ 6. Deeper observations targeting low-mass galaxies will be required to confirm this finding. [ABSTRACT FROM AUTHOR]

Published
2020
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70. Molecular gas content in obscured AGN at z > 1

Author

Perna, M., primary, Sargent, M. T., additional, Brusa, M., additional, Daddi, E., additional, Feruglio, C., additional, Cresci, G., additional, Lanzuisi, G., additional, Lusso, E., additional, Comastri, A., additional, Coogan, R. T., additional, D’Amato, Q., additional, Gilli, R., additional, Piconcelli, E., additional, and Vignali, C., additional

Published
2018
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73. Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2

Author

Strazzullo, V., primary, Coogan, R. T., additional, Daddi, E., additional, Sargent, M. T., additional, Gobat, R., additional, Valentino, F., additional, Bethermin, M., additional, Pannella, M., additional, Dickinson, M., additional, Renzini, A., additional, Arimoto, N., additional, Cimatti, A., additional, Dannerbauer, H., additional, Finoguenov, A., additional, Liu, D., additional, and Onodera, M., additional

Published
2018
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74. Merger driven star-formation activity in Cl J1449+0856 at z=1.99 as seen by ALMA and JVLA

Author

Coogan, R T, primary, Daddi, E, additional, Sargent, M T, additional, Strazzullo, V, additional, Valentino, F, additional, Gobat, R, additional, Magdis, G, additional, Bethermin, M, additional, Pannella, M, additional, Onodera, M, additional, Liu, D, additional, Cimatti, A, additional, Dannerbauer, H, additional, Carollo, M, additional, Renzini, A, additional, and Tremou, E, additional

Published
2018
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75. Molecular outflow and feedback in the obscured quasar XID2028 revealed by ALMA

Author

Brusa, M., primary, Cresci, G., additional, Daddi, E., additional, Paladino, R., additional, Perna, M., additional, Bongiorno, A., additional, Lusso, E., additional, Sargent, M. T., additional, Casasola, V., additional, Feruglio, C., additional, Fraternali, F., additional, Georgiev, I., additional, Mainieri, V., additional, Carniani, S., additional, Comastri, A., additional, Duras, F., additional, Fiore, F., additional, Mannucci, F., additional, Marconi, A., additional, Piconcelli, E., additional, Zamorani, G., additional, Gilli, R., additional, La Franca, F., additional, Lanzuisi, G., additional, Lutz, D., additional, Santini, P., additional, Scoville, N. Z., additional, Vignali, C., additional, Vito, F., additional, Rabien, S., additional, Busoni, L., additional, and Bonaglia, M., additional

Published
2018
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76. Red, redder, reddest: SCUBA-2 imaging of colour-selected Herschel sources

Author

Duivenvoorden, S, primary, Oliver, S, additional, Scudder, J M, additional, Greenslade, J, additional, Riechers, D A, additional, Wilkins, S M, additional, Buat, V, additional, Chapman, S C, additional, Clements, D L, additional, Cooray, A, additional, Coppin, K E K, additional, Dannerbauer, H, additional, De Zotti, G, additional, Dunlop, J S, additional, Eales, S A, additional, Efstathiou, A, additional, Farrah, D, additional, Geach, J E, additional, Holland, W S, additional, Hurley, P D, additional, Ivison, R J, additional, Marchetti, L, additional, Petitpas, G, additional, Sargent, M T, additional, Scott, D, additional, Symeonidis, M, additional, Vaccari, M, additional, Vieira, J D, additional, Wang, L, additional, Wardlow, J, additional, and Zemcov, M, additional

Published
2018
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77. Deciphering the Activity and Quiescence of High-redshift Cluster Environments:ALMA Observations of Cl J1449+0856 at z=2

Author

Strazzullo, V., Coogan, R. T., Daddi, E., Sargent, M. T., Gobat, R., Valentino, F., Bethermin, M., Pannella, M., Dickinson, M., Renzini, A., Arimoto, N., Cimatti, A., Dannerbauer, H., Finoguenov, A., Liu, D., Onodera, M., Strazzullo, V., Coogan, R. T., Daddi, E., Sargent, M. T., Gobat, R., Valentino, F., Bethermin, M., Pannella, M., Dickinson, M., Renzini, A., Arimoto, N., Cimatti, A., Dannerbauer, H., Finoguenov, A., Liu, D., and Onodera, M.

Published
2018

78. The dust attenuation of star‐forming galaxies at z similar to 3 and beyond: New insights from ALMA observations

Author

Fudamoto, Y., Oesch, P. A., Schinnerer, E., Groves, B., Karim, A., Magnelli, B., Sargent, M. T., Cassata, P., Lang, P., Liu, D., Le Fevre, O., Leslie, S., Smolcic, V., Tasca, L., 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), and 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)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract

International audience; We present results on the dust attenuation of galaxies at redshift similar to 3‐6 by studying the relationship between the UV spectral slope (beta(UV)) and the infrared excess (IRX; L‐IR/L‐UV) using Atacama Large Millimeter/submillimeter Array (ALMA) far‐infrared continuum observations. Our study is based on a sample of 67 massive, star‐forming galaxies with a median mass of M‐* similar to 10(10.7) M‐circle dot spanning a redshift range z = 2.6‐3.7 (median z = 3.2) that were observed with ALMA at lambda(rest) = 300 mu m. Both the individual ALMA detections (41 sources) and stacks including all galaxies show the IRX‐beta(UV) relationship at z similar to 3 is mostly consistent with that of local starburst galaxies on average. However, we find evidence for a large dispersion around the mean relationship by up to +/‐ 0.5 dex. Nevertheless, the locally calibrated dust correction factors based on the IRX‐beta(UV) relation are on average applicable to main‐sequence z similar to 3 galaxies. This does not appear to be the case at even higher redshifts, however. Using public ALMA observations of z similar to 4‐6 galaxies we find evidence for a significant evolution in the IRX‐beta(UV) and the IRX‐M‐* relations beyond z similar to 3 towards lower IRX values. We discuss several caveats that could affect these results, including the assumed dust temperature. ALMA observations of larger z > 3 galaxy sample spanning a wide range of physical parameters (e.g. lower stellar mass) will be important to investigate this intriguing redshift evolution further.

Published
2017
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79. Radio Selection of the Most Distant Galaxy Clusters

Author

Daddi, E., primary, Jin, S., additional, Strazzullo, V., additional, Sargent, M. T., additional, Wang, T., additional, Ferrari, C., additional, Schinnerer, E., additional, Smolčić, V., additional, Calabró, A., additional, Coogan, R., additional, Delhaize, J., additional, Delvecchio, I., additional, Elbaz, D., additional, Gobat, R., additional, Gu, Q., additional, Liu, D., additional, Novak, M., additional, and Valentino, F., additional

Published
2017
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80. The dust attenuation of star-forming galaxies at z ∼ 3 and beyond: New insights from ALMA observations

Author

Fudamoto, Y., primary, Oesch, P. A., additional, Schinnerer, E., additional, Groves, B., additional, Karim, A., additional, Magnelli, B., additional, Sargent, M. T., additional, Cassata, P., additional, Lang, P., additional, Liu, D., additional, Le Fèvre, O., additional, Leslie, S., additional, Smolčić, V., additional, and Tasca, L., additional

Published
2017
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81. ALMA constraints on star-forming gas in a prototypical z = 1.5 clumpy galaxy: the dearth of CO(5−4) emission from UV-bright clumps

Author

Cibinel, A., primary, Daddi, E., additional, Bournaud, F., additional, Sargent, M. T., additional, le Floc'h, E., additional, Magdis, G. E., additional, Pannella, M., additional, Rujopakarn, W., additional, Juneau, S., additional, Zanella, A., additional, Duc, P.-A., additional, Oesch, P. A., additional, Elbaz, D., additional, Jagannathan, P., additional, Nyland, K., additional, and Wang, T., additional

Published
2017
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82. GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR-RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z similar or equal to 4

Author

Pannella, M., Elbaz, D., Daddi, Emanuele, Dickinson, M., Hwang, H. S., Schreiber, C., Strazzullo, V., Aussel, H., Bethermin, M., Buat, V., Charmandaris, V., Cibinel, A., Juneau, S., Ivison, R. J., Le Borgne, Damien, Le Floc'H, E., Leiton, R., Lin, L., Magdis, G., Morrison, G. E., Mullaney, J., Onodera, M., Renzini, A., Salim, S., Sargent, M. T., Scott, D., Shu, X., Wang, T., 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), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, National Optical Astronomy Observatory (NOAO), Korea Institute for Advanced Study (KIAS), Ludwig-Maximilians-Universität München (LMU), 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), Observatoire de Paris, Université Paris sciences et lettres (PSL), University of Crete [Heraklion] (UOC), Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing [Penteli] (IAASARS), National Observatory of Athens (NOA), Royal Observatory Edinburgh (ROE), University of Edinburgh, Universidad de Concepción - University of Concepcion [Chile], Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), 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), NOAO, 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), PSL Research University (PSL), Ecosystèmes lagunaires : organisation biologique et fonctionnement (ECOLAG), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Centre National de la Recherche Scientifique (CNRS), Universidad de Concepción [Chile], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Pannella, M, Elbaz, D, Daddi, E, Dickinson, M, Hwang, H, Schreiber, C, Strazzullo, V, Aussel, H, Bethermin, M, Buat, V, Charmandaris, V, Cibinel, A, Juneau, S, Ivison, Rj, Le Borgne, D, Le Floc'h, E, Leiton, R, Lin, L, Magdis, G, Morrison, Ge, Mullaney, J, Onodera, M, Renzini, A, Salim, S, Sargent, Mt, Scott, D, Shu, X, and Wang, T

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; We use deep panchromatic data sets in the GOODS-N field, from GALEX to the deepest Herschel far-infrared (FIR) and VLA radio continuum imaging, to explore the evolution of star-formation activity and dust attenuation properties of star-forming galaxies to z similar or equal to 4, using mass-complete samples. Our main results can be summarized as follows: (i) the slope of the star-formation rate-M* correlation is consistent with being constant similar or equal to 0.8 up to z similar or equal to 1.5, while its normalization keeps increasing with redshift; (ii) for the first time we are able to explore the FIR-radio correlation for a mass-selected sample of star-forming galaxies: the correlation does not evolve up to z similar or equal to 4; (iii) we confirm that galaxy stellar mass is a robust proxy for UV dust attenuation in star-forming galaxies, with more massive galaxies being more dust attenuated. Strikingly, we find that this attenuation relation evolves very weakly with redshift, with the amount of dust attenuation increasing by less than 0.3 mag over the redshift range [0.5-4] for a fixed stellar mass; (iv) the correlation between dust attenuation and the UV spectral slope evolves with redshift, with the median UV slope becoming bluer with redshift. By z similar or equal to 3, typical UV slopes are inconsistent, given the measured dust attenuations, with the predictions of commonly used empirical laws. (v) Finally, building on existing results, we show that gas reddening is marginally larger (by a factor of around 1.3) than the stellar reddening at all redshifts probed. Our results support a scenario where the ISM conditions of typical star-forming galaxies evolve with redshift, such that at z \textgreater= 1.5 Main Sequence galaxies have ISM conditions moving closer to those of local starbursts.

Published
2015
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88. HELP: star formation as a function of galaxy environment withHerschel

Author

Duivenvoorden, S., primary, Oliver, S., additional, Buat, V., additional, Darvish, B., additional, Efstathiou, A., additional, Farrah, D., additional, Griffin, M., additional, Hurley, P. D., additional, Ibar, E., additional, Jarvis, M., additional, Papadopoulos, A., additional, Sargent, M. T., additional, Scott, D., additional, Scudder, J. M., additional, Symeonidis, M., additional, Vaccari, M., additional, Viero, M. P., additional, and Wang, L., additional

Published
2016
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89. The contribution of starbursts and normal galaxies to IR luminosity functions and the molecular gas content of the Universe at z<2

Author

Sargent, M T, Daddi, E, Béthermin, M, and Elbaz, D

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QB
Abstract

We present a parameter-less approach capable of predicting\ud the shape of the infrared luminosity function at redshifts z ≤2. It relies on\ud three observables: (1) the redshift evolution of the stellar mass function\ud for star-forming galaxies, (2) the evolution of the specific star formation\ud rate of main-sequence galaxies, and (3) the double-Gaussian decomposition\ud of the specific star formation rate distribution at fixed stellar mass\ud into the contributions (assumed to be redshift- and mass-invariant) from\ud main-sequence and starburst activity.\ud Using this self-consistent and simple framework, we identify the contributions\ud of main-sequence and starburst activity to the global infrared luminosity\ud function and find a constant or only weakly redshift-dependent\ud contribution (8–14%) of starbursts to the star formation rate density at\ud z ≤2. Over the same redshift range, we also infer the evolution of the\ud cosmic abundance of molecular gas in star-forming galaxies, based on the\ud relations between star formation rate and molecular gas mass followed by\ud normal and starburst galaxies.

Published
2013

90. GOODS-Herschel : the far-infrared view of star formation in active galactic nucleus host galaxies since z ≈ 3

Author

Mullaney, J. R., Pannella, M., Daddi, E., Alexander, D. M., Elbaz, D., Hickox, R. C., Bournaud, F., Altieri, B., Aussel, H., Coia, D., Dannerbauer, H., Dasyra, K., Dickinson, M., Hwang, H. S., Kartaltepe, J., Leiton, R., Magdis, G., Magnelli, B., Popesso, P., Valtchanov, I., Bauer, F. E., Brandt, W. N., Del Moro, A., Hanish, D. J., Ivison, R. J., Juneau, S., Luo, B., Lutz, D., Sargent, M. T., Scott, D., and Xue, Y. Q.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present a study of the infrared properties of X-ray selected, moderate-luminosity (i.e. LX= 1042–1044 erg s−1) active galactic nuclei (AGNs) up to z ≈ 3, in order to explore the links between star formation in galaxies and accretion on to their central black holes. We use 100 and 160 μ m fluxes from GOODS-Herschel – the deepest survey yet undertaken by the Herschel telescope – and show that in the vast majority of cases (i.e. >94 per cent) these fluxes are dominated by emission from the host galaxy. As such, these far-infrared bands provide an uncontaminated view of star formation in the AGN host galaxies. We find no evidence of any correlation between the X-ray and infrared luminosities of moderate AGNs at any redshift, suggesting that global star formation is decoupled from nuclear (i.e. AGN) activity in these galaxies. On the other hand, we confirm that the star formation rates of AGN hosts increase strongly with redshift, by a factor of 43+27− 18 from z < 0.1 to z = 2–3 for AGNs with the same range of X-ray luminosities. This increase is entirely consistent with the factor of 25–50 increase in the specific star formation rates (SSFRs) of normal, star-forming (i.e. main-sequence) galaxies over the same redshift range. Indeed, the average SSFRs of AGN hosts are only marginally (i.e. ≈20 per cent) lower than those of main-sequence galaxies at all surveyed redshifts, with this small deficit being due to a fraction of AGNs residing in quiescent (i.e. low SSFR) galaxies. We estimate that 79 ± 10 per cent of moderate-luminosity AGNs are hosted in main-sequence galaxies, 15 ± 7 per cent in quiescent galaxies and

Published
2012

91. COLDz: Karl G. Jansky Very Large Array discovery of a gas-rich galaxy in COSMOS

Author

Lentati, Lindley, Wagg, J., Carilli, C L, Riechers, Dominik, Capak, P, Walter, F., Aravena, M., da Cunha, Elisabete, Hodge, J. A., Ivison, R. J, Smail, Ian, Sharon, C., Daddi, E, Decarli, Roberto, Dickinson, Mark, Sargent, M. T., Scoville, Nick, Smolcic, Vernesa, Lentati, Lindley, Wagg, J., Carilli, C L, Riechers, Dominik, Capak, P, Walter, F., Aravena, M., da Cunha, Elisabete, Hodge, J. A., Ivison, R. J, Smail, Ian, Sharon, C., Daddi, E, Decarli, Roberto, Dickinson, Mark, Sargent, M. T., Scoville, Nick, and Smolcic, Vernesa

Published
2015

92. GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TOz≃ 4

Author

Pannella, M., primary, Elbaz, D., additional, Daddi, E., additional, Dickinson, M., additional, Hwang, H. S., additional, Schreiber, C., additional, Strazzullo, V., additional, Aussel, H., additional, Bethermin, M., additional, Buat, V., additional, Charmandaris, V., additional, Cibinel, A., additional, Juneau, S., additional, Ivison, R. J., additional, Borgne, D. Le, additional, Floc’h, E. Le, additional, Leiton, R., additional, Lin, L., additional, Magdis, G., additional, Morrison, G. E., additional, Mullaney, J., additional, Onodera, M., additional, Renzini, A., additional, Salim, S., additional, Sargent, M. T., additional, Scott, D., additional, Shu, X., additional, and Wang, T., additional

Published
2015
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94. No Evolution in the IR–Radio Relation for IR-luminous Galaxies at z < 2 in the COSMOS Field

Author

Sargent, M. T., Schinnerer, E., Murphy, E., Carilli, C. L., Helou, G., Aussel, H., Le Floc'h, E., Frayer, D. T., Ilbert, O., Oesch, P., Salvato, M., Smolčić, V., Kartaltepe, J., and Sanders, D. B.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Previous observational studies of the infrared (IR)-radio relation out to high redshift employed any detectable star-forming systems at a given redshift within the restricted area of cosmological survey fields. Consequently, the evolution inferred relies on a comparison between the average IR/radio properties of (1) very IR-luminous high-z sources and (2) more heterogeneous low(er)-z samples that often lack the strongest IR emitters. In this Letter, we consider populations of objects with comparable luminosities over the last 10 Gyr by taking advantage of deep IR (especially Spitzer 24 μm) and Very Large Array 1.4 GHz observations of the COSMOS field. Consistent with recent model predictions, both Ultra Luminous Infrared Galaxies and galaxies on the bright end of the evolving IR luminosity function do not display any change in their average IR/radio ratios out to z ~ 2 when corrected for bias. Uncorrected data suggested ~0.3 dex of positive evolution.

Published
2010

95. Evidence for feedback in action from the molecular gas content in thez~ 1.6 outflowing QSO XID2028

Author

Brusa, M., primary, Feruglio, C., additional, Cresci, G., additional, Mainieri, V., additional, Sargent, M. T., additional, Perna, M., additional, Santini, P., additional, Vito, F., additional, Marconi, A., additional, Merloni, A., additional, Lutz, D., additional, Piconcelli, E., additional, Lanzuisi, G., additional, Maiolino, R., additional, Rosario, D., additional, Daddi, E., additional, Bongiorno, A., additional, Fiore, F., additional, and Lusso, E., additional

Published
2015
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96. TheHerschelview of the dominant mode of galaxy growth fromz= 4 to the present day

Author

Schreiber, C., primary, Pannella, M., additional, Elbaz, D., additional, Béthermin, M., additional, Inami, H., additional, Dickinson, M., additional, Magnelli, B., additional, Wang, T., additional, Aussel, H., additional, Daddi, E., additional, Juneau, S., additional, Shu, X., additional, Sargent, M. T., additional, Buat, V., additional, Faber, S. M., additional, Ferguson, H. C., additional, Giavalisco, M., additional, Koekemoer, A. M., additional, Magdis, G., additional, Morrison, G. E., additional, Papovich, C., additional, Santini, P., additional, and Scott, D., additional

Published
2015
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97. The Dependence of Star Formation Activity on Stellar Mass Surface Density and Sersic Index in zCOSMOS Galaxies at 0.5

Author

Maier, C., Lilly, S. J., Zamorani, G., Scodeggio, M., Lamareille, F., Contini, T., Sargent, M. T., Scarlata, C., Oesch, P., Carollo, C. M., Fevre, O. Le, Renzini, A., Kneib, J. -P., Mainieri, V., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Coppa, G., Cucciati, O., De La Torre, S., De Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Kovac, K., Borgne, J. -F. Le, Brun, V. Le, Mignoli, M., Pello, R., Peng, Y., Montero, E. Perez, Ricciardelli, E., Silverman, J. D., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Abbas, U., Bottini, D., Cappi, A., Cassata, P., Cimatti, Alessandro, Fumana, M., Guzzo, L., Halliday, C., Leauthaud, A., Maccagni, D., Marinoni, Christian, McCracken, H. J., Memeo, P., Meneux, B., Porciani, C., Pozzetti, L., Scaramella, R., Walcher, J., Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

One of the key unanswered questions in the study of galaxy evolution is what physical processes inside galaxies drive the changes in the SFRs in individual galaxies that, taken together, produce the large decline in the global star-formation rate density (SFRD) to redshifts since z~2. Many studies of the SFR at intermediate redshifts have been made as a function of the integrated stellar mass of galaxies but these did not use information on the internal structural properties of the galaxies. In this paper we present a comparative study of the dependence of SFRs on the average surface mass densities (SigmaM) of galaxies of different morphological types up to z~1 using the zCOSMOS and SDSS surveys. The main findings about the evolution of these relatively massive galaxies are: 1) There is evidence that, for both SDSS ans zCOSMOS galaxies, the mean specific SFR within a given population (either disk-dominated or bulge-dominated) is independent of SigmaM; 2) The observed SSFR - SigmaM step-function relation is due, at all investigated redshifts, to the changing mix of disk-dominated and bulge-dominated galaxies as surface density increases and the strong difference in the average SSFR between disks and bulges. We also find a modest differential evolution in the size-mass relations of disk and spheroid galaxies; 3) The shape of the median SSFR - SigmaM relation is similar, but with median SSFR values that are about 5-6 times higher in zCOSMOS galaxies than for SDSS, across the whole range of SigmaM, and in both spheroid and disk galaxies. This increase matches that of the global SFRD of the Universe as a whole, emphasizing that galaxies of all types are contributing, proportionally, to the global increase in SFRD in the Universe back to these redshifts (abridged)., Published 2009 in ApJ, 694, 1099

Published
2009

98. ALMA constraints on star-forming gas in a prototypical z = 1.5 clumpy galaxy: the dearth of CO(5-4) emission from UV-bright clumps.

Author

Cibinel, A., Daddi, E., Bournaud, F., Sargent, M. T., le Floc'h, E., Magdis, G. E., Pannella, M., Rujopakarn, W., Juneau, S., Zanella, A., Duc, P.-A., Oesch, P. A., Elbaz, D., Jagannathan, P., Nyland, K., and Wang, T.

Subjects
GALACTIC evolution, STELLAR populations, STELLAR density (Stellar population), STAR formation
Abstract

We present deep ALMA CO(5-4) observations of a main-sequence, clumpy galaxy at z = 1.5 in the HUDF. Thanks to the ∼0″.5 resolution of the ALMA data, we can link stellar population properties to the CO(5-4) emission on scales of a few kiloparsec. We detect strong CO(5-4) emission from the nuclear region of the galaxy, consistent with the observed LIR-L'CO(5-4) correlation and indicating ongoing nuclear star formation. The CO(5-4) gas component appears more concentrated than other star formation tracers or the dust distribution in this galaxy. We discuss possible implications of this difference in terms of star formation efficiency and mass build-up at the galaxy centre. Conversely, we do not detect any CO(5-4) emission from the UV-bright clumps. This might imply that clumps have a high star formation efficiency (although they do not display unusually high specific star formation rates) and are not entirely gas dominated, with gas fractions no larger than that of their host galaxy (∼50 per cent). Stellar feedback and disc instability torques funnelling gas towards the galaxy centre could contribute to the relatively low gas content. Alternatively, clumps could fall in a more standard star formation efficiency regime if their actual star formation rates are lower than generally assumed. We find that clump star formation rates derived with several different, plausible methods can vary by up to an order of magnitude. The lowest estimates would be compatible with a CO(5-4) non-detection even for main-sequence like values of star formation efficiency and gas content. [ABSTRACT FROM AUTHOR]

Published
2017
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99. The environmental effect on galaxy evolution: Cl J1449 + 0856 at z = 1.99.

Author

Coogan, Rosemary T., Daddi, E., Gobat, R., Sargent, M. T., Bergmann, Thaisa Storchi, Forman, William, Overzier, Roderik, and Riffel, Rogério

Abstract

This work focuses on understanding the formation of the first massive, passive galaxies in clusters, as a first step to the development of environmental trends seen at low redshift. Cl J1449 + 0856 is an excellent case to study this - a galaxy cluster at redshift z = 1.99 that already shows evidence of a virialised atmosphere. Here we highlight two recent results: the discovery of merger-driven star formation and highly-excited molecular gas in galaxies at the core of Cl J1449, along with the lowest-mass Sunyaev-Zel'dovich detection to date. [ABSTRACT FROM AUTHOR]

Published
2019
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100. Dust and gas in luminous proto-cluster galaxies at z=4.05: the case for different cosmic dust evolution in normal and starburst galaxies

Author

Tan, Q., Daddi, E, Magdis, G., Pannella, M, Sargent, M. T., Riechers, Dominik, Bethermin, M, Bournaud, F., Carilli, C L, da Cunha, Elisabete, Dannerbauer, Helmut, Tan, Q., Daddi, E, Magdis, G., Pannella, M, Sargent, M. T., Riechers, Dominik, Bethermin, M, Bournaud, F., Carilli, C L, da Cunha, Elisabete, and Dannerbauer, Helmut

Abstract

We measure the dust and gas content of the three submillimeter galaxies (SMGs) in the GN20 proto-cluster at z = 4.05 using new IRAM Plateau de Bure interferometer (PdBI) CO(4–3) and 1.2–3.3 mm continuum observations. All these three SMGs are heavily dust obscured, with UV-based star formation rate (SFR) estimates significantly smaller than the ones derived from the bolometric infrared (IR), consistent with the spatial offsets revealed by HST and CO imaging. Based also on evaluations of the specific SFR, CO-to-H2 conversion factor and gas depletion timescale, we classify all the three galaxies as starbursts (SBs), although with a lower confidence for GN20.2b that might be a later stage merging event. We place our measurements in the context of the evolutionary properties of main sequence (MS) and SB galaxies. ULIRGs have 3–5 times larger L CO/Mdust and Mdust/M ratios than z = 0 MS galaxies, but by z ∼ 2 the difference appears to be blurred, probably due to differential metallicity evolution. SB galaxies appear to slowly evolve in their L CO/Mdust and Mdust/M ratios all the way to z > 6 (consistent with rapid enrichment of SB events), while MS galaxies rapidly increase in Mdust/M from z = 0 to 2 (due to gas fraction increase, compensated by a decrease of metallicities). While no IR/submm continuum detection is available for indisputably normal massive galaxies at z > 2.5, we show that if metallicity indeed decrease rapidly for these systems at z > 3 as claimed in the literature, we should expect a strong decrease of their Mdust/M, consistent with recent PdBI and ALMA upper limits. We conclude that the Mdust/M ratio could be a powerful tool for distinguishing starbursts from normal galaxies at z > 4. Key w

Published
2014

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