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20 results on '"Genzel, R."'

1. PHIBSS2: survey design and z = 0.5 – 0.8 results: Molecular gas reservoirs during the winding-down of star formation.

Author

Freundlich, J., Combes, F., Tacconi, L. J., Genzel, R., Garcia-Burillo, S., Neri, R., Contini, T., Bolatto, A., Lilly, S., Salomé, P., Bicalho, I. C., Boissier, J., Boone, F., Bouché, N., Bournaud, F., Burkert, A., Carollo, M., Cooper, M. C., Cox, P., and Feruglio, C.

Subjects
STAR formation, GAS reservoirs, REDSHIFT, GALAXIES
Abstract

Following the success of the Plateau de Bure high-z Blue Sequence Survey (PHIBSS), we present the PHIBSS2 legacy program, a survey of the molecular gas properties of star-forming galaxies on and around the star-formation main sequence (MS) at different redshifts using IRAM's NOrthern Extended Millimeter Array (NOEMA). This survey significantly extends the existing sample of star-forming galaxies with CO molecular gas measurements, probing the peak epoch of star formation (z = 1 − 1.6) as well as its building-up (z = 2 − 3) and winding-down (z = 0.5 − 0.8) phases. The targets are drawn from the well-studied GOODS, COSMOS, and AEGIS cosmological deep fields and uniformly sample the MS in the stellar mass (M⋆) – star formation rate (SFR) plane with log(M⋆/M⊙) = 10 − 11.8 and SFR = 3.5 − 500 M⊙ yr−1 without morphological selection, thus providing a statistically meaningful census of star-forming galaxies at different epochs. We describe the survey strategy and sample selection before focusing on the results obtained at redshift z = 0.5 − 0.8, where we report 60 CO(2-1) detections out of 61 targets. We determine molecular gas masses between 2 × 109 and 5 × 1010 M⊙ and separately obtain disc sizes and bulge-to-total (B/T) luminosity ratios from HST I-band images. The median molecular gas-to-stellar mass ratio μgas∼ = 0.28 ± 0.04 μ gas ∼ = 0.28 ± 0.04 $ \widetilde{\mu_{\mathrm{gas}}} = 0.28 \pm 0.04 $ , gas fraction fgas∼ = 0.22 ± 0.02 f gas ∼ = 0.22 ± 0.02 $ \widetilde{f_{\mathrm{gas}}} = 0.22 \pm 0.02 $ , and depletion time t depl ∼ = 0.84 ± 0.07 Gyr $ \widetilde{t_{\mathrm{depl}}} = 0.84 \pm 0.07\,\mathrm{Gyr} $ as well as their dependence with stellar mass and offset from the MS follow published scaling relations for a much larger sample of galaxies spanning a significantly wider range of redshifts, the cosmic evolution of the SFR being mainly driven by that of the molecular gas fraction. The galaxy-averaged molecular Kennicutt–Schmidt (KS) relation between molecular gas and SFR surface densities is strikingly linear, pointing towards similar star formation timescales within galaxies at any given epoch. In terms of morphology, the molecular gas content, the SFR, the disc stellar mass, and the disc molecular gas fraction do not seem to correlate with B/T and the stellar surface density, which suggests an ongoing supply of fresh molecular gas to compensate for the build-up of the bulge. Our measurements do not yield any significant variation of the depletion time with B/T and hence no strong evidence for morphological quenching within the scatter of the MS. [ABSTRACT FROM AUTHOR]

Published
2019
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2. The evolution of the dust and gas content in galaxies.

Author

Santini, P., Maiolino, R., Magnelli, B., Lutz, D., Lamastra, A., Li Causi, G., Eales, S., Andreani, P., Berta, S., Buat, V., Cooray, A., Cresci, G., Daddi, E., Farrah, D., Fontana, A., Franceschini, A., Genzel, R., Granato, G., Grazian, A., and Le Floc'h, E.

Subjects
GALACTIC evolution, REDSHIFT, INFRARED astronomy, COSMIC rays, STELLAR activity, ASTRONOMY
Abstract

We use deep Herschel observations taken with both PACS and SPIRE imaging cameras to estimate the dust mass of a sample of galaxies extracted from the GOODS-S, GOODS-N and the COSMOS fields. We divide the redshift-stellar mass (Mstar)-star formation rate (SFR) parameter space into small bins and investigate average properties over this grid. In the first part of the work we investigate the scaling relations between dust mass, stellar mass and SFR out to z = 2.5. No clear evolution of the dust mass with redshift is observed at a given SFR and stellar mass. We find a tight correlation between the SFR and the dust mass, which, under reasonable assumptions, is likely a consequence of the Schmidt-Kennicutt (S-K) relation. The previously observed correlation between the stellar content and the dust content flattens or sometimes disappears when considering galaxies with the same SFR. Our finding suggests that most of the correlation between dust mass and stellar mass obtained by previous studies is likely a consequence of the correlation between the dust mass and the SFR combined with the main sequence, i.e., the tight relation observed between the stellar mass and the SFR and followed by the majority of star-forming galaxies. We then investigate the gas content as inferred from dust mass measurements. We convert the dust mass into gas mass by assuming that the dust-to-gas ratio scales linearly with the gas metallicity (as supported by many observations). For normal star-forming galaxies (on the main sequence) the inferred relation between the SFR and the gas mass (integrated S-K relation) broadly agrees with the results of previous studies based on CO measurements, despite the completely different approaches. We observe that all galaxies in the sample follow, within uncertainties, the same S-K relation. However, when investigated in redshift intervals, the S-K relation shows a moderate, but significant redshift evolution. The bulk of the galaxy population at z ∼ 2 converts gas into stars with an efficiency (star formation efficiency, SFE = SFR/Mgas, equal to the inverse of the depletion time) about 5 times higher than at z ∼ 0. However, it is not clear what fraction of such variation of the SFE is due to an intrinsic redshift evolution and what fraction is simply a consequence of high-z galaxies having, on average, higher SFR, combined with the super-linear slope of the S-K relation (while other studies find a linear slope). We confirm that the gas fraction ( fgas = Mgas/(Mgas + Mstar)) decreases with stellar mass and increases with the SFR. We observe no evolution with redshift once Mstar and SFR are fixed. We explain these trends by introducing a universal relation between gas fraction, stellar mass and SFR that does not evolve with redshift, at least out to z ∼ 2.5. Galaxies move across this relation as their gas content evolves across the cosmic epochs. We use the 3D fundamental fga-Mstar-SFR relation, along with the evolution of the main sequence with redshift, to estimate the evolution of the gas fraction in the average population of galaxies as a function of redshift and as a function of stellar mass: we find that Mstar >⩾ 1011 M☉ galaxies show the strongest evolution at z ≳ 1.3 and a flatter trend at lower redshift, while fgas decreases more regularly over the entire redshift range probed in Mstar ≲1011 M☉ galaxies, in agreement with a downsizing scenario. [ABSTRACT FROM AUTHOR]

Published
2014
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3. Evidence of strong quasar feedback in the early Universe.

Author

Maiolino, R., Gallerani, S., Neri, R., Cicone, C., Ferrara, A., Genzel, R., Lutz, D., Sturm, E., Tacconi, L. J., Walter, F., Feruglio, C., Fiore, F., and Piconcelli, E.

Subjects
QUASARS, MATHEMATICAL models, GALACTIC evolution, REDSHIFT, SUPERGIANT stars, STELLAR populations
Abstract

ABSTRACT Most theoretical models invoke quasar-driven outflows to quench star formation in massive galaxies, and this feedback mechanism is required to account for the population of old and passive galaxies observed in the local Universe. The discovery of massive, old and passive galaxies at z∼ 2 implies that such quasar feedback on to the host galaxy must have been at work very early on, close to the reionization epoch. We have observed the [C ii] 158 m transition in SDSS J114816.64+525150.3, which, at z= 6.4189, is one of the most distant quasars known. We detect broad wings of the line tracing a quasar-driven massive outflow. This is the most distant massive outflow ever detected and is likely tracing the long-sought quasar feedback, already at work in the early Universe. The outflow is marginally resolved on scales of ∼16 kpc, implying that the outflow can really affect the whole galaxy, as required by quasar feedback models. The inferred outflow rate, , is the highest ever found. At this rate, the outflow can clean the gas in the host galaxy, and therefore quench star formation, in a few million years. [ABSTRACT FROM AUTHOR]

Published
2012
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4. THE METALLICITY DEPENDENCE OF THE CO → H2 CONVERSION FACTOR IN z ≥ 1 STAR-FORMING GALAXIES.

Author

Genzel, R., Tacconi, L. J., Combes, F., Bolatto, A., Neri, R., Sternberg, A., Cooper, M. C., Bouchié, N., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Schreiber, N. M. Förster, García-Burillo, S., Gracia-Carpio, J., Lutz, O., Naab, T., Newman, S., and Saintonge, A.

Subjects
*GALAXY formation, *ULTRAVIOLET radiation, *REDSHIFT, *STELLAR mass, *ASTROPHYSICS
Abstract

We use the first systematic samples of CO millimeter emission in z ≥ 1 "main-sequence" star-forming galaxies to study the metallicity dependence of the conversion factor αCO, from CO line luminosity to molecular gas mass. The molecular gas depletion rate inferred from the ratio of the star formation rate (SFR) to CO luminosity, is ~1 Gyr-1 for near-solar metallicity galaxies with stellar masses above Ms ~ 101l M⊙. In this regime, the depletion rate does not vary more than a factor of two to three as a function of molecular gas surface density or redshift between z ~ 0 and 2. Below Ms the depletion rate increases rapidly with decreasing metallicity. We argue that this trend is not caused by starburst events, by changes in the physical parameters of the molecular clouds, or by the impact of the fundamental-metallicity-SFR-stellar mass relation. A more probable explanation is that the conversion factor is metallicity dependent and that star formation can occur in "CO-dark" gas. The trend is also expected theoretically from the effect of enhanced photodissociation of CO by ultraviolet radiation at low metallicity. From the available z ~ 0 and z ~ 1-3 samples we constrain the slope of the log(αCO)-log (metallicity) relation to range between -1 and -2, fairly insensitive to the assumed slope of the gas-SFR relation. Because of the lower metallicities near the peak of the galaxy formation activity at z ~ 1-2 compared to z ~ 0, we suggest that molecular gas masses estimated from CO luminosities have to be substantially corrected upward for galaxies below Ms. [ABSTRACT FROM AUTHOR]

Published
2012
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5. A study of the gas–star formation relation over cosmic time.

Author

Genzel, R., Tacconi, L. J., Gracia-Carpio, J., Sternberg, A., Cooper, M. C., Shapiro, K., Bolatto, A., Bouché, N., Bournaud, F., Burkert, A., Combes, F., Comerford, J., Cox, P., Davis, M., Schreiber, N. M. Förster, Garcia-Burillo, S., Lutz, D., Naab, T., Neri, R., and Omont, A.

Subjects
*ASTRONOMICAL research, *STAR formation, *GALACTIC evolution, *STARBURSTS, *REDSHIFT, *ACCRETION (Astrophysics), *INTERSTELLAR medium
Abstract

We use the first systematic data sets of CO molecular line emission in z∼ 1–3 normal star-forming galaxies (SFGs) for a comparison of the dependence of galaxy-averaged star formation rates on molecular gas masses at low and high redshifts, and in different galactic environments. Although the current high- z samples are still small and biased towards the luminous and massive tail of the actively star-forming ‘main-sequence’, a fairly clear picture is emerging. Independent of whether galaxy-integrated quantities or surface densities are considered, low- and high- z SFG populations appear to follow similar molecular gas–star formation relations with slopes 1.1 to 1.2, over three orders of magnitude in gas mass or surface density. The gas-depletion time-scale in these SFGs grows from 0.5 Gyr at to 1.5 Gyr at . The average corresponds to a fairly low star formation efficiency of 2 per cent per dynamical time. Because star formation depletion times are significantly smaller than the Hubble time at all redshifts sampled, star formation rates and gas fractions are set by the balance between gas accretion from the halo and stellar feedback. In contrast, very luminous and ultraluminous, gas-rich major mergers at both low and high z produce on average four to 10 times more far-infrared luminosity per unit gas mass. We show that only some fraction of this difference can be explained by uncertainties in gas mass or luminosity estimators; much of it must be intrinsic. A possible explanation is a top-heavy stellar mass function in the merging systems but the most likely interpretation is that the star formation relation is driven by global dynamical effects. For a given mass, the more compact merger systems produce stars more rapidly because their gas clouds are more compressed with shorter dynamical times, so that they churn more quickly through the available gas reservoir than the typical normal disc galaxies. When the dependence on galactic dynamical time-scale is explicitly included, disc galaxies and mergers appear to follow similar gas-to-star formation relations. The mergers may be forming stars at slightly higher efficiencies than the discs. [ABSTRACT FROM AUTHOR]

Published
2010
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6. A search for neutral carbon towards two z= 4.05 submillimetre galaxies, GN 20 and GN 20.2.

Author

Casey, C. M., Chapman, S. C., Daddi, E., Dannerbauer, H., Pope, A., Scott, D., Bertoldi, F., Beswick, R. J., Blain, A. W., Cox, P., Genzel, R., Greve, T. R., Ivison, R. J., Muxlow, T. W. B., Neri, R., Omont, A., Smail, I., and Tacconi, L. J.

Subjects
GALAXIES, CARBON, ASTRONOMY, MILKY Way, REDSHIFT
Abstract

Using the IRAM Plateau de Bure Interferometer (PdBI) we have searched for the upper fine structure line of neutral carbon [ ] and towards the submillimetre galaxies (SMGs) GN 20 (SMM J123711.9+622212, ) and GN 20.2 (SMM J123708.8+622202, ). The far-infrared continuum is detected at 8σ significance in GN 20, with a flux density of , while no continuum is detected in GN 20.2. Both sources are statistically undetected in both and lines; we derive line luminosity limits for both C i and CO of . Assuming carbon excitation temperatures of (the galaxies' measured dust temperatures), we infer C i mass limits of (GN 20) and . The derived C i abundance limits are for GN 20 and for GN 20.2, implying that the systems have Milky Way level carbon enrichment ( X[C i]/ X[H2]) or lower, similar to high-redshift carbon-detected systems (at ) but about 50 times less than the carbon enrichment of local starburst galaxies. Observations of GN 20 and GN 20.2 in high-resolution MERLIN+VLA (Multi-Element Radio Linked Interferometer Network+Very Large Array) radio maps of GOODS-N (Great Observatories Origin Deep Survey-North) are used to further constrain the sizes and locations of active regions. We conclude that the physical gas properties of young rapidly evolving systems like GN 20 and GN 20.2 are likely significantly different than starburst/ULIRG (ultraluminous infrared galaxy) environments in the local Universe yet similar to SMGs. Unless gravitationally amplified examples can be found, observations of galaxies like GN 20 will require the order of magnitude increase in sensitivity of the Atacama Large Millimetre Array (ALMA) to constrain their C i and high- J CO content, despite the fact that they are the brightest systems at . [ABSTRACT FROM AUTHOR]

Published
2009
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7. The evolution and origin of ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS3D

Author

T. Taro Shimizu, Ken-ichi Tadaki, Linda J. Tacconi, Maximilian Fabricius, Rebecca L. Davies, Stijn Wuyts, David J. Wilman, Sedona H. Price, Pieter van Dokkum, Natascha M. Förster Schreiber, Audrey Galametz, A. Beifiori, Reinhard Genzel, Jeffrey C. C. Chan, Richard Davies, Rodrigo Herrera-Camus, Thorsten Naab, Matteo Fossati, Sirio Belli, Emily Wisnioski, Gabriel Brammer, Philipp Lang, J. Trevor Mendel, Ralf Bender, Erica J. Nelson, Roberto P. Saglia, Ivelina Momcheva, Andreas Burkert, Dieter Lutz, Hannah Übler, Ubler, H, Genzel, R, Wisnioski, E, Schreiber, N, Shimizu, T, Price, S, Tacconi, L, Belli, S, Wilman, D, Fossati, M, Mendel, J, Davies, R, Beifiori, A, Bender, R, Brammer, G, Burkert, A, Chan, J, Fabricius, M, Galametz, A, Herrera-Camus, R, Lang, P, Lutz, D, Momcheva, I, Naab, T, Nelson, E, Saglia, R, Tadaki, K, Dokkum, P, and Wuyts, S

Subjects
010504 meteorology & atmospheric sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gravitation, galaxies: high-redshift, Ionization, 0103 physical sciences, kinematics and dynamics [galaxies], Galaxy formation and evolution, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, ISM [galaxies], Velocity dispersion, Sigma, Astronomy and Astrophysics, Galaxy, Redshift, Accretion (astrophysics), Space and Planetary Science, galaxies: evolution, galaxies: ISM, high-redshift [galaxies]
Abstract

We present the 0.6 < z < 2.6 evolution of the ionized gas velocity dispersion in 175 star-forming disk galaxies based on data from the full integral field spectroscopic survey. In a forward-modeling Bayesian framework including instrumental effects and beam-smearing, we fit simultaneously the observed galaxy velocity and velocity dispersion along the kinematic major axis to derive the intrinsic velocity dispersion σ 0. We find a reduction of the average intrinsic velocity dispersion of disk galaxies as a function of cosmic time, from σ 0 ∼ 45 km s -1 at z ∼ 2.3 to σ 0 ∼ 30 km s -1 at z ∼ 0.9. There is substantial intrinsic scatter (σ σ0,int ≈ 10km s -1) around the best-fit σ 0-z relation beyond what can be accounted for from the typical measurement uncertainties (δσ 0 ≈ 12 km s -1), independent of other identifiable galaxy parameters. This potentially suggests a dynamic mechanism such as minor mergers or variation in accretion being responsible for the scatter. Putting our data into the broader literature context, we find that ionized and atomic+molecular velocity dispersions evolve similarly with redshift, with the ionized gas dispersion being ∼10-15 km s -1 higher on average. We investigate the physical driver of the on average elevated velocity dispersions at higher redshift and find that our galaxies are at most marginally Toomre-stable, suggesting that their turbulent velocities are powered by gravitational instabilities, while stellar feedback as a driver alone is insufficient. This picture is supported through comparison with a state-of-the-art analytical model of galaxy evolution.

Published
2019

8. The evolution of the Tully-Fisher relation between z~2.3 and z~0.9 with KMOS^3D

Author

N. M. Förster Schreiber, Emily Wisnioski, Erica J. Nelson, P. G. van Dokkum, M. H. Fabricius, R. D. Davies, Stijn Wuyts, A. Burkert, Reinhard Genzel, D. Wilman, R. Bender, Dieter Lutz, Audrey Galametz, G. B. Brammer, Hannah Übler, I. Momcheva, Ken-ichi Tadaki, R. P. Saglia, Jeffrey C. C. Chan, T. Naab, Linda J. Tacconi, Matteo Fossati, S. Belli, Philipp Lang, A. Beifiori, Stella Seitz, J. T. Mendel, Ubler, H, Forster Schreiber, N, Genzel, R, Wisnioski, E, Wuyts, S, Lang, P, Naab, T, Burkert, A, Van Dokkum, P, Tacconi, L, Wilman, D, Fossati, M, Mendel, J, Beifiori, A, Belli, S, Bender, R, Brammer, G, Chan, J, Davies, R, Fabricius, M, Galametz, A, Lutz, D, Momcheva, I, Nelson, E, Saglia, R, Seitz, S, and Tadaki, K

Subjects
Stellar mass, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Tully–Fisher relation, 01 natural sciences, Gravitational potential, Evolution [Galaxies], High-Redshift [Galaxies], 0103 physical sciences, Galaxies: Evolution, Galaxy formation and evolution, Galaxies: Kinematics And Dynamics, Kinematics And Dynamics [Galaxies], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies: High-Redshift, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo
Abstract

We investigate the stellar mass and baryonic mass Tully-Fisher relations (TFRs) of massive star-forming disk galaxies at redshift z~2.3 and z~0.9 as part of the KMOS^3D integral field spectroscopy survey. Our spatially resolved data allow reliable modelling of individual galaxies, including the effect of pressure support on the inferred gravitational potential. At fixed circular velocity, we find higher baryonic masses and similar stellar masses at z~2.3 as compared to z~0.9. Together with the decreasing gas-to-stellar mass ratios with decreasing redshift, this implies that the contribution of dark matter to the dynamical mass at the galaxy scale increases towards lower redshift. A comparison to local relations reveals a negative evolution of the stellar and baryonic TFR zero-points from z=0 to z~0.9, no evolution of the stellar TFR zero-point from z~0.9 to z~2.3, and a positive evolution of the baryonic TFR zero-point from z~0.9 to z~2.3. We discuss a toy model of disk galaxy evolution to explain the observed, non-monotonic TFR evolution, taking into account the empirically motivated redshift dependencies of galactic gas fractions, and of the relative amount of baryons to dark matter on galaxy and halo scales., 27 pages, 14 figures, accepted for publication in ApJ

Published
2017

9. Galaxy environment in the 3D-HST fields. Witnessing the onset of satellite quenching at z ~ 1-2

Author

Rosalind E. Skelton, Philipp Lang, Jeffrey C. C. Chan, Ralf Bender, Erica J. Nelson, Matteo Fossati, J. T. Mendel, Stijn Wuyts, Katherine E. Whitaker, Roberto P. Saglia, David J. Wilman, Ken-ichi Tadaki, Linda J. Tacconi, Gabriel B. Brammer, Emily Wisnioski, Richard Davies, K. Bandara, Reinhard Genzel, William G. Hartley, I. G. Momcheva, Audrey Galametz, N. M. Förster Schreiber, H. Übler, M. Fabricius, Eva Wuyts, Alessandra Beifiori, P. G. van Dokkum, Sandesh K. Kulkarni, Fossati, M, Wilman, D, Mendel, J, Saglia, R, Galametz, A, Beifiori, A, Bender, R, Chan, J, Fabricius, M, Bandara, K, Brammer, G, Davies, R, Forster Schreiber, N, Genzel, R, Hartley, W, Kulkarni, S, Lang, P, Momcheva, I, Nelson, E, Skelton, R, Tacconi, L, Tadaki, K, Ubler, H, Van Dokkum, P, Wisnioski, E, Whitaker, K, Wuyts, E, and Wuyts, S

Subjects
Stellar mass, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, Satellite galaxy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, methods: statistical, 010308 nuclear & particles physics, Star formation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Galaxy, Redshift, Space and Planetary Science, galaxies: star formation, Astrophysics of Galaxies (astro-ph.GA), galaxies: statistic, Halo, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract

We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-HST/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multi wavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than $JH_{140} < 24$ mag in the redshift range $0.5, Comment: 35 pages, 29 figures, 2 tables. Accepted for publication in ApJ. The catalogue of environmental measures is available at: http://dx.doi.org/10.5281/zenodo.168056

Published
2016
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10. The KMOS3D Survey: Design, First Results, and the Evolution of Galaxy Kinematics from 0.7≤ z ≤ 2.7

Author

G. B. Brammer, K. Bandara, Stijn Wuyts, R. D. Davies, N. M. Förster Schreiber, M. H. Fabricius, P. G. van Dokkum, E. Wuyts, S. R. Kulkarni, Jeffrey C. C. Chan, Erica J. Nelson, D. Wilman, Emily Wisnioski, I. Momcheva, Matteo Fossati, Dieter Lutz, R. Genzel, R. Bender, R. P. Saglia, David J. Rosario, Y. Fudamoto, J. D. Kurk, Stella Seitz, Linda J. Tacconi, J. T. Mendel, Philipp Lang, A. Beifiori, Wisnioski, E, Forster Schreiber, N, Wuyts, S, Wuyts, E, Bandara, K, Wilman, D, Genzel, R, Bender, R, Davies, R, Fossati, M, Lang, P, Mendel, J, Beifiori, A, Brammer, G, Chan, J, Fabricius, M, Fudamoto, Y, Kulkarni, S, Kurk, J, Lutz, D, Nelson, E, Momcheva, I, Rosario, D, Saglia, R, Seitz, S, Tacconi, L, and Van Dokkum, P

Subjects
Physics, Velocity dispersion, Astronomy and Astrophysics, Survey research, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, Field survey, Astrophysics - Astrophysics of Galaxies, galaxies [infrared], Galaxy, Redshift, infrared: galaxies, Space and Planetary Science, galaxies: high-redshift, kinematics and dynamics [galaxies], galaxies: kinematics and dynamic, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics, evolution [galaxies], high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the KMOS^3D survey, a new integral field survey of over 600 galaxies at 0.71$, implying that the star-forming 'main sequence' (MS) is primarily composed of rotating galaxies at both redshift regimes. When considering additional stricter criteria, the Halpha kinematic maps indicate at least ~70% of the resolved galaxies are disk-like systems. Our high-quality KMOS data confirm the elevated velocity dispersions reported in previous IFS studies at z>0.7. For rotation-dominated disks, the average intrinsic velocity dispersion decreases by a factor of two from 50 km/s at z~2.3 to 25 km/s at z~0.9 while the rotational velocities at the two redshifts are comparable. Combined with existing results spanning z~0-3, disk velocity dispersions follow an approximate (1+z) evolution that is consistent with the dependence of velocity dispersion on gas fractions predicted by marginally-stable disk theory., Comment: 20 pages, 11 figures, 1 Appendix; Accepted to ApJ November 25

Published
2015

11. The evolution of the dust and gas content in galaxies

Author

Filippo Mannucci, Giulia Rodighiero, Georgios E. Magdis, Laura Silva, Paola Santini, Duncan Farrah, Steve Eales, Giovanni Cresci, Andrea Grazian, L. Riguccini, Francesca Pozzi, A. Cooray, Reinhard Genzel, David J. Rosario, G. Li Causi, Benjamin Magnelli, S. Berta, E. Le Floc'h, Kevin Xu, Seb Oliver, Adriano Fontana, Alberto Franceschini, Linda J. Tacconi, Manuela Magliocchetti, A. Lamastra, Gian Luigi Granato, Paola Popesso, Marco P. Viero, Emanuele Daddi, Raanan Nordon, Roberto Maiolino, Stijn Wuyts, V. Buat, Paola Andreani, Douglas Scott, Mara Salvato, Nicola Menci, Dieter Lutz, Lingyu Wang, INAF - Osservatorio Astrofisico di Arcetri (OAA), 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), 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, Santini, P., Maiolino, R., Magnelli, B., Lutz, D., Lamastra, A., Li Causi, G., Eales, S., Andreani, P., Berta, S., Buat, V., Cooray, A., Cresci, G., Daddi, E., Farrah, D., Fontana, A., Franceschini, A., Genzel, R., Granato, G., Grazian, A., Le Floc'H, E., Magdis, G., Magliocchetti, M., Mannucci, F., Menci, N., Nordon, R., Oliver, S., Popesso, P., Pozzi, F., Riguccini, L., Rodighiero, G., Rosario, D.J., Salvato, M., Scott, D., Silva, L., Tacconi, L., Viero, M., Wang, L., Wuyts, S., Xu, K., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared: galaxie, Metallicity, astro-ph.GA, Population, Galaxies: fundamental parameter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, galaxies [infrared], Universal relation, infrared: galaxies, QB0460, galaxies: high-redshift, Astrophysics::Solar and Stellar Astrophysics, fundamental parameters [galaxies], education, Scaling, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Physics, education.field_of_study, ISM [galaxies], infrared galaxies, Astronomy and Astrophysics, galaxies: fundamental parameters, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Content (measure theory), astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astronomical and Space Sciences, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use deep Herschel PACS and SPIRE observations in GOODSS, GOODSN and COSMOS to estimate the average dust mass (Mdust) of galaxies on a redshift-stellar mass (Mstar)-SFR grid. We study the scaling relations between Mdust, Mstar and SFR at z, Accepted for publication in A&A

Published
2014

12. A Consistent Study of Metallicity Evolution at 0.8 < z < 2.6

Author

Ric Davies, Sandesh K. Kulkarni, Pieter G. van Dokkum, Linda J. Tacconi, Jeffrey C. C. Chan, Thorsten Naab, Erica J. Nelson, Matteo Fossati, Amiel Sternberg, Stijn Wuyts, David J. Wilman, Eva Wuyts, Reinhard Genzel, Ivelina Momcheva, J. Trevor Mendel, Jaron Kurk, Ray M. Sharples, Andreas Burkert, Stella Seitz, Chiara Mancini, Roberto P. Saglia, Dieter Lutz, Gabriel B. Brammer, K. Bandara, Simon J. Lilly, Philipp Lang, Ralf Bender, Emily Wisnioski, Alessandra Beifiori, Sandro Tacchella, C. Marcella Carollo, Alvio Renzini, David J. Rosario, Natascha M. Förster Schreiber, P. Buschkamp, Frank Eisenhauer, Wuyts, E, Kurk, J, Forster Schreiber, N, Genzel, R, Wisnioski, E, Bandara, K, Wuyts, S, Beifiori, A, Bender, R, Brammer, G, Burkert, A, Buschkamp, P, Carollo, C, Chan, J, Davies, R, Eisenhauer, F, Fossati, M, Kulkarni, S, Lang, P, Lilly, S, Lutz, D, Mancini, C, Mendel, J, Momcheva, I, Naab, T, Nelson, E, Renzini, A, Rosario, D, Saglia, R, Seitz, S, Sharples, R, Sternberg, A, Tacchella, S, Tacconi, L, Van Dokkum, P, and Wilman, D

Subjects
Luminous infrared galaxy, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Star formation, Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, infrared: galaxies, high-redshift [Galaxies], Stars, Space and Planetary Science, galaxies: high-redshift, galaxies. [Infrared], Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution, Stellar evolution, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the correlations between stellar mass, star formation rate (SFR) and [NII]/Ha flux ratio as indicator of gas-phase metallicity for a sample of 222 galaxies at 0.8 < z < 2.6 and log(M*/Msun)=9.0-11.5 from the LUCI, SINS/zC-SINF and KMOS3D surveys. This sample provides a unique analysis of the mass-metallicity relation (MZR) over an extended redshift range using consistent data analysis techniques and strong-line metallicity indicator. We find a constant slope at the low-mass end of the relation and can fully describe its redshift evolution through the evolution of the characteristic turnover mass where the relation begins to flatten at the asymptotic metallicity. At fixed mass and redshift, our data do not show a correlation between the [NII]/Ha ratio and SFR, which disagrees with the 0.2-0.3dex offset in [NII]/Ha predicted by the "fundamental relation" between stellar mass, SFR and metallicity discussed in recent literature. However, the overall evolution towards lower [NII]/Ha at earlier times does broadly agree with these predictions., 7 pages, 4 figures, ApJ, 789, L40

Published
2014
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13. THE EVOLUTION OF METALLICITY AND METALLICITY GRADIENTS FROMz= 2.7 TO 0.6 WITH KMOS3D

Author

Hannah Übler, Ric Davies, Stella Seitz, Natascha M. Förster Schreiber, Ken-ichi Tadaki, Alessandra Beifiori, Gabriel B. Brammer, Ivelina Momcheva, Jeffrey C. C. Chan, Pieter van Dokkum, Sandesh K. Kulkarni, Linda J. Tacconi, Sirio Belli, David J. Wilman, Andreas Burkert, Matteo Fossati, Ralf Bender, Dieter Lutz, Erica J. Nelson, Roberto P. Saglia, Audrey Galametz, David J. Rosario, Stijn Wuyts, Thorsten Naab, Emily Wisnioski, J. Trevor Mendel, Bernhard Röttgers, Philipp Lang, K. Bandara, E. Wuyts, Reinhard Genzel, Wuyts, E, Wisnioski, E, Fossati, M, Schreiber, N, Genzel, R, Davies, R, Mendel, J, Naab, T, Rottgers, B, Wilman, D, Wuyts, S, Bandara, K, Beifiori, A, Belli, S, Bender, R, Brammer, G, Burkert, A, Chan, J, Galametz, A, Kulkarni, S, Lang, P, Lutz, D, Momcheva, I, Nelson, E, Rosario, D, Saglia, R, Seitz, S, Tacconi, L, Tadaki, K, Ubler, H, and Dokkum, P

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Stellar mass, Stellar population, Metallicity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, galaxies: abundance, galaxies: high-redshift, abundances [galaxies], 0103 physical sciences, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Effective radius, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present measurements of the [NII]/Ha ratio as a probe of gas-phase oxygen abundance for a sample of 419 star-forming galaxies at z=0.6-2.7 from the KMOS3D near-IR multi-IFU survey. The mass-metallicity relation (MZR) is determined consistently with the same sample selection, metallicity tracer, and methodology over the wide redshift range probed by the survey. We find good agreement with long-slit surveys in the literature, except for the low-mass slope of the relation at z~2.3, where this sample is less biased than previous samples based on optical spectroscopic redshifts. In this regime we measure a steeper slope than some literature results. Excluding the AGN contribution from the MZR reduces sensitivity at the high mass end, but produces otherwise consistent results. There is no significant dependence of the [NII]/Ha ratio on SFR or environment at fixed redshift and stellar mass. The IFU data allow spatially resolved measurements of [NII]/Ha, from which we can infer abundance gradients for 180 galaxies, thus tripling the current sample in the literature. The observed gradients are on average flat, with only 15 gradients statistically offset from zero at >3sigma. We have modelled the effect of beam-smearing, assuming a smooth intrinsic radial gradient and known seeing, inclination and effective radius for each galaxy. Our seeing-limited observations can recover up to 70% of the intrinsic gradient for the largest, face-on disks, but only 30% for the smaller, more inclined galaxies. We do not find significant trends between observed or corrected gradients and any stellar population, dynamical or structural galaxy parameters, mostly in agreement with existing studies with much smaller sample sizes. In cosmological simulations, strong feedback is generally required to produce flat gradients at high redshift., submitted to ApJ

Published
2016

14. The Impact of Evolving Infrared Spectral Energy Distributions of Galaxies on Star Formation Rate Estimates

Author

Emanuele Daddi, Roberto Maiolino, Herve Aussel, Dieter Lutz, Ivan Valtchanov, Paola Popesso, Alessandro Cimatti, Albrecht Poglitsch, Amélie Saintonge, Reinhard Genzel, Stijn Wuyts, S. Berta, Francesca Pozzi, Bruno Altieri, A. M. Pérez García, David J. Rosario, M. Sanchez-Portal, Guilaine Lagache, Linda J. Tacconi, Giulia Rodighiero, Ángel Bongiovanni, Jordi Cepa, N. M. Förster Schreiber, Raanan Nordon, Lin Yan, Dario Fadda, P. Santini, E. Sturm, Benjamin Magnelli, Paola Andreani, Nordon R., Lutz D., Genzel R., Berta S., Wuyts S., Magnelli B., Altieri B., Andreani P., Aussel H., Bongiovanni A., Cepa J., Cimatti A., Daddi E., Fadda D., Förster Schreiber N. M., Lagache G., Maiolino R., Pérez García A. M., Poglitsch A., Popesso P., Pozzi F., Rodighiero G., Rosario D., Saintonge A., Sanchez-Portal M., Santini P., Sturm E., Tacconi L. J., Valtchanov I., and Yan L.

Subjects
Physics, cosmology: observation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Infrared, Star formation, Spectral density, FOS: Physical sciences, galaxies: starburst, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Spectral line, Galaxy, infrared: galaxies, Space and Planetary Science, Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, galaxies: fundamental parameter, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We combine Herschel-PACS data from the PEP program with Spitzer 24 um and 16 um photometry and ultra deep IRS mid-infrared spectra, to measure the mid- to far-infrared spectral energy distribution (SED) of 0.7, Comment: 25 pages, 15 figures, accepted to ApJ; v3 include many minor modifications following the referee report, added a section comparing various z~2 IR template calibrations

Published
2012

15. The lesser role of starbursts in star formation at $z=2$

Author

P. Andreani, P. Santini, Georgios E. Magdis, E. Le Floc'h, G. Rodighiero, Roberto Maiolino, Alvio Renzini, M. Magliocchetti, Ivano Baronchelli, Alberto Franceschini, Adriano Fontana, Antonio Cava, L. Riguccini, Linda J. Tacconi, Francesca Pozzi, Dieter Lutz, P. Popesso, Stijn Wuyts, S. Berta, G. Zamorani, E. Daddi, Albrecht Poglitsch, A. Grazian, O. Ilbert, Carlotta Gruppioni, Anna Feltre, Raanan Nordon, N. M. Förster Schreiber, Benjamin Magnelli, H. Aussel, D. Elbaz, H. J. McCracken, Reinhard Genzel, A. Cimatti, Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Dipartimento di Fisica e Astronomia [Bologna], Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Extraterrestrische Physik (MPE), European Southern Observatory (ESO), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Dipartimento di Fisica [Povo], Università degli Studi di Trento (UNITN), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), 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), ANR-08-JCJC-0008,UPGAL(2008), European Project: 240039,EC:FP7:ERC,ERC-2009-StG,UPGAL(2009), Universita degli Studi di Padova, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Rodighiero G., Daddi E., Baronchelli I., Cimatti A., Renzini A., Aussel H., Popesso P., Lutz D., Andreani P., Berta S., Cava A., Elbaz D., Feltre A., Fontana A., Förster Schreiber N. M., Franceschini A., Genzel R., Grazian A., Gruppioni C., Ilbert O., Le Floch E., Magdis G., Magliocchetti M., Magnelli B., Maiolino R., McCracken H., Nordon R., Poglitsch A., Santini P., Pozzi F., Riguccini L., Tacconi L. J., Wuyts S., Zamorani G., Dipartimento di Astronomia, 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), Università di Bologna [Bologna] (UNIBO), Departamento de Astrofisica, Universidad Complutense de Madrid [Madrid] (UCM), INAF - Osservatorio Astronomico (OAR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and UPGAL

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Morphological transformation, Critical phase, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, galaxies: interactions, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Conjunction (astronomy), Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Galaxy, Redshift, Space and Planetary Science, galaxies: interaction, Astrophysics::Earth and Planetary Astrophysics, galaxies: nuclei, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Two main modes of star formation are know to control the growth of galaxies: a relatively steady one in disk-like galaxies, defining a tight star formation rate (SFR)-stellar mass sequence, and a starburst mode in outliers to such a sequence which is generally interpreted as driven by merging. Such starburst galaxies are rare but have much higher SFRs, and it is of interest to establish the relative importance of these two modes. PACS/Herschel observations over the whole COSMOS and GOODS-South fields, in conjunction with previous optical/near-IR data, have allowed us to accurately quantify for the first time the relative contribution of the two modes to the global SFR density in the redshift interval 1.51000M(sun)/yr, off-sequence sources significantly contribute to the SFR density (46+/-20%). We conclude that merger-driven starbursts play a relatively minor role for the formation of stars in galaxies, whereas they may represent a critical phase towards the quenching of star formation and morphological transformation in galaxies., Comment: Accepted for publication in ApJ Letters

Published
2011

16. The SINS Survey: Modeling the Dynamics of z ~ 2 Galaxies and the High-z Tully-Fisher Relation

Author

Emanuele Daddi, S. L. Lilly, Shy Genel, Karina Caputi, Erin K. S. Hicks, Jaron Kurk, P. Buschkamp, Thorsten Naab, Ortwin Gerhard, Andreas Burkert, Giovanni Cresci, N. M. Foerster Schreiber, Dieter Lutz, Amiel Sternberg, Charles C. Steidel, Reinhard Genzel, Ric Davies, Kristen L. Shapiro, Alice E. Shapley, Frank Eisenhauer, Nicolas Bouché, Linda J. Tacconi, Dawn K. Erb, Alvio Renzini, Jesper Sommer-Larsen, Andrea Cimatti, Cresci G., Hicks E. K. S., Genzel R., Schreiber N. M. Förster, Davies R., Bouché N., Buschkamp P., Genel S., Shapiro K., Tacconi L., Sommer-Larsen J., Burkert A., Eisenhauer F., Gerhard O., Lutz D., Naab T., Sternberg A., Cimatti A., Daddi E., Erb D. K., Kurk J., Lilly S. L., Renzini A., Shapley A., Steidel C. C., Caputi K., and Astronomy

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, H-ALPHA, INTERMEDIATE REDSHIFT, FOS: Physical sciences, Zero-point energy, Angular velocity, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Tully–Fisher relation, HIGH-REDSHIFT GALAXIES, infrared: galaxies, galaxies: high-redshift, STAR-FORMING GALAXIES, STELLAR MASS DENSITY, INTEGRAL FIELD SPECTROSCOPY, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Physics, ADAPTIVE OPTICS, Astronomy and Astrophysics, DISK GALAXIES, Galaxy, Redshift, Accretion (astrophysics), LYMAN-BREAK GALAXIES, Space and Planetary Science, ROTATION CURVES, Astrophysics::Earth and Planetary Astrophysics, Halo, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the modeling of SINFONI integral field dynamics of 18 star forming galaxies at z ~ 2 from Halpha line emission. The galaxies are selected from the larger sample of the SINS survey, based on the prominence of ordered rotational motions with respect to more complex merger induced dynamics. The quality of the data allows us to carefully select systems with kinematics dominated by rotation, and to model the gas dynamics across the whole galaxy using suitable exponential disk models. We obtain a good correlation between the dynamical mass and the stellar mass, finding that large gas fractions Mgas~M*) are required to explain the difference between the two quantities. We use the derived stellar mass and maximum rotational velocity Vmax from the modeling to construct for the first time the stellar mass Tully-Fisher relation at z ~ 2.2. The relation obtained shows a slope similar to what is observed at lower redshift, but we detect an evolution of the zero point. We find that at z ~ 2.2 there is an offset in log(M*) for a given rotational velocity of 0.41+-0.11 with respect to the local Universe. This result is consistent with the predictions of the latest N-body/hydrodynamical simulations of disk formation and evolution, which invoke gas accretion onto the forming disk in filaments and cooling flows. This scenario is in agreement with other dynamical evidence from SINS, where gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z ~ 2 galaxies., Comment: 10 pages, 6 figures, submitted to ApJ

Published
2009

17. The European Large-Area ISO Survey (ELAIS): the final band-merged catalogue

Author

M. Rowan-Robinson, C. Lari, I. Perez-Fournon, E. A. Gonzalez-Solares, F. La Franca, M. Vaccari, S. Oliver, C. Gruppioni, P. Ciliegi, P. Héraudeau, S. Serjeant, A. Efstathiou, T. Babbedge, I. Matute, F. Pozzi, A. Franceschini, P. Vaisanen, A. Afonso-Luis, D. M. Alexander, O. Almaini, A. C. Baker, S. Basilakos, M. Barden, C. del Burgo, I. Bellas-Velidis, F. Cabrera-Guerra, R. Carballo, C. J. Cesarsky, D. L. Clements, H. Crockett, L. Danese, A. Dapergolas, B. Drolias, N. Eaton, E. Egami, D. Elbaz, D. Fadda, M. Fox, R. Genzel, P. Goldschmidt, J. I. Gonzalez-Serrano, M. Graham, G. L. Granato, E. Hatziminaoglou, U. Herbstmeier, M. Joshi, E. Kontizas, M. Kontizas, J. K. Kotilainen, D. Kunze, A. Lawrence, D. Lemke, M. J. D. Linden-Vørnle, R. G. Mann, I. Márquez, J. Masegosa, R. G. McMahon, G. Miley, V. Missoulis, B. Mobasher, T. Morel, H. Nørgaard-Nielsen, A. Omont, P. Papadopoulos, J.-L. Puget, D. Rigopoulou, B. Rocca-Volmerange, N. Sedgwick, L. Silva, T. Sumner, C. Surace, B. Vila-Vilaro, P. van der Werf, A. Verma, L. Vigroux, M. Villar-Martin, C. J. Willott, A. Carramiñana, R. Mujica, Universidad de Cantabria, Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, AUTRES, Space Telescope Science Institute (STSci), Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Fisica de Plasmas (GoLP), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Imperial College London, 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), Oxford Astrophysics, Instituto de Astrofisica de Canarias (IAC), Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Laboratoire de Physico-Chimie des Polymères et des Milieux Dispersés (PPMD), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Laboratoire de thermodynamique et physico-chimie métallurgiques (LTPCM), Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), 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 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), University of Oxford, 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), Università degli Studi di Padova = University of Padua (Unipd), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-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), Department of Physics, Dipartimento di Astronomia, Université Pierre et Marie Curie - Paris 6 (UPMC)-ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute, Rowan-Robinson M., Lari C., Perez-Fournon I., Gonzalez-Solares E. A., La Franca F., Vaccari M., Oliver S., Gruppioni C., Ciliegi P., Héraudeau P., Serjeant S., Efstathiou A., Babbedge T., Matute I., Pozzi F., Franceschini A., Vaisanen P., Afonso-Luis A., Alexander D. M., Almaini O., Baker A. C., Basilakos S., Barden M., del Burgo C., Bellas-Velidis I., Cabrera-Guerra F., Carballo R., Cesarsky C. J., Clements D. L., Crockett H., Danese L., Dapergolas A., Drolias B., Eaton N., Egami E., Elbaz D., Fadda D., Fox M., Genzel R., Goldschmidt P., Gonzalez-Serrano J. I., Graham M., Granato G. L., Hatziminaoglou E., Herbstmeier U., Joshi M., Kontizas E., Kontizas M., Kotilainen J. K., Kunze D., Lawrence A., Lemke D., Linden-Vørnle M. J. D., Mann R. G., Márquez I., Masegosa J., McMahon R. G., Miley G., Missoulis V., Mobasher B., Morel T., Nørgaard-Nielsen H., Omont A., Papadopoulos P., Puget J.-L., Rigopoulou D., Rocca-Volmerange B., Sedgwick N., Silva L., Sumner T., Surace C., Vila-Vilaro B., van der Werf P., Verma A., Vigroux L., Villar-Martin M., Willott C. J., Carramiñana A., and Mujica R.

Subjects
010504 meteorology & atmospheric sciences, galaxies : evolution, Infrared, galaxies: starburst, Astrophysics, HUBBLE-DEEP-FIELD, 01 natural sciences, X-RAY SURVEY, SOUTHERN FIELD, galaxies [Infrared], EXTRAGALACTIC SOURCE COUNTS, Astrophysics::Solar and Stellar Astrophysics, observations [Cosmology], 010303 astronomy & astrophysics, formation [Stars], Physics, infrared : galaxies, stars : formation, Astrophysics (astro-ph), STAR-FORMATION HISTORY, FORMATION RATES, cosmology : observations, Cirrus, galaxies : starburst, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, ACTIVE GALACTIC NUCLEI, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, infrared: galaxies, 0103 physical sciences, 170 MU-M, DATA REDUCTION, [INFO]Computer Science [cs], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Luminous infrared galaxy, stars: formation, Spectral density, Astronomy and Astrophysics, Torus, Quasar, evolution [Galaxies], Redshift, Galaxy, starburst [Galaxies], Space and Planetary Science, cosmology: observations, HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present the final band-merged ELAIS catalogue at 6.7, 15, 90, and 175 $��$m, and the associated data at u,g,r,i,z,J,H,K, and 20cm. The origin of the survey, infrared and radio observations, data-reduction and optical identifications are briefly reviewed, and a summary of the area covered, and completeness limit for each infrared band is given. A detailed discussion of the band-merging and optical association strategy is given. The total catalogues consists of 2860 sources. For extragalactic sources observed in 3 or more infrared bands, colour-colour diagrams are presented and discussed in terms of the contributing infrared populations. Spectral energy distributions are shown for selected sources and compared with cirrus, M82 and Arp220 starburst, and AGN dust torus models. Spectroscopic redshifts are tabulated, where available. For the N1 and N2 areas, the INT ugriz Wide Field Survey, permits photometric redshifts to be estimated for galaxies and quasars. These agree well with the spectroscopic redshifts, within the uncertainty of the photometric method. The redshift distribution is given for selected ELAIS bands and colour-redshift diagrams are discussed. There is a high proportion of ultraluminous infrared galaxies in the ELAIS Catalogue ($> 10 %$ of 15 $��$m sources), many with Arp220-like colours. 10 hyperluminous infrared galaxies and 10 EROs are found in the survey. The large numbers of ultraluminous galaxies imply very strong evolution in the star-formation rate between z = 0 and 1., 21 pages, 31 figures. Accepted for publication in MNRAS

Published
2004

18. The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

Author

Andrea Biviano, David Elbaz, Giulia Rodighiero, Antonio Cava, Kim-Vy Tran, Carlotta Gruppioni, Dario Fadda, Paola Popesso, Dieter Lutz, Ivan Valtchanov, Kalliopi Dasyra, Helmut Dannerbauer, Francesca Pozzi, S. Berta, Lijing Shao, Alexis Finoguenov, E. Le Floc'h, Jeyhan S. Kartaltepe, D. Coia, Amélie Saintonge, Ho Seong Hwang, Shannon G. Patel, L. Riguccini, Raanan Nordon, N. M. Förster Schreiber, Ivano Baronchelli, Albrecht Poglitsch, Paola Andreani, Reinhard Genzel, Benjamin Magnelli, O. Ilbert, Linda J. Tacconi, Roger Leiton, Bruno Altieri, Andrea Cimatti, Mara Salvato, E. Daddi, Herve Aussel, M. Sanchez Portal, Mark Dickinson, Adam Tomczak, Georgios E. Magdis, Peter Capak, Popesso P., Biviano A., Rodighiero G., Baronchelli I., Salvato M., Saintonge A., Finoguenov A., Magnelli B., Gruppioni C., Pozzi F., Lutz D., Elbaz D., Altieri B., Andreani P., Aussel H., Berta S., Capak P., Cava A., Cimatti A., Coia D., Daddi E., Dannerbauer H., Dickinson M., Dasyra K., Fadda D., Förster Schreiber N., Genzel R., Hwang H. S., Kartaltepe J., Ilbert O., Le Floch E., Leiton R., Magdis, G., Nordon R., Patel S., Poglitsch A., Riguccini L., Sanchez Portal M., Shao L., Tacconi L., Tomczak A., Tran K., and Valtchanov I.

Subjects
Physics, Luminous infrared galaxy, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, galaxies: clusters: general, galaxies: high-redshift, Space and Planetary Science, Galaxy group, galaxies: evolution, education, Low Mass, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Star formation in massive galaxies is quenched at some point during hierarchical mass assembly. To understand where and when the quenching processes takes place, we study the evolution of the total star formation rate per unit total halo mass (\Sigma(SFR/M)) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift ~1.6. We use deep far-infrared PACS data at 100 and 160 um to accurately estimate the total star formation rate of the Luminous Infrared Galaxy population of 9 clusters with mass ~10^{15} M_{\odot}, and 9 groups/poor clusters with mass ~ 5 x 10^{13} M_{\odot}. Estimates of the field \Sigma(SFR/M) are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe. The field \Sigma(SFR/M) increases with redshift up to z~1 and it is constant thereafter. The evolution of the \Sigma(SFR/M)-z relation in galaxy systems is much faster than in the field. Up to redshift z~0.2, the field has a higher \Sigma(SFR/M) than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar \Sigma(SFR/M), while massive clusters have significantly lower \Sigma(SFR/M) than both groups and the field. There is a hint of a reversal of the SFR activity vs. environment at z~1.6, where the group \Sigma(SFR/M) lies above the field \Sigma(SFR/M)-z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching., Comment: 8 pages, 3 figures, accepted for publication on A&A

Published
2012

19. Building the cosmic infrared background brick by brick withHerschel/PEP

Author

Bruno Altieri, Albrecht Poglitsch, Stijn Wuyts, Linda J. Tacconi, Ivan Valtchanov, Raanan Nordon, Miguel Sánchez-Portal, Paola Andreani, N. M. Foerster Schreiber, J. Cepa, Reinhard Genzel, E. Le Floc'h, Giulia Rodighiero, E. Sturm, Benjamin Magnelli, Herve Aussel, Francesca Pozzi, Ismael Perez-Fournon, Andrea Cimatti, S. Berta, Héctor O. Castañeda, Paola Popesso, David Elbaz, L. Riguccini, Dieter Lutz, Emanuele Daddi, Roberto Maiolino, Berta S., Magnelli B., Nordon R., Lutz D., Wuyts S., Altieri B., Andreani P., Aussel H., Castañeda H., Cepa J., Cimatti A., Daddi E., Elbaz D., Förster Schreiber N. M., Genzel R., Le Floc'h E., Maiolino R., Pérez-Fournon I., Poglitsch A., Popesso P., Pozzi F., Riguccini L., Rodighiero G., Sanchez-Portal M., Sturm E., Tacconi L. J., and Valtchanov I.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, infrared: galaxie, FOS: Physical sciences, Flux, Astronomy and Astrophysics, cosmic background radiation, Astrophysics, infrared: diffuse background, Galaxy, Redshift, Wavelength, Space and Planetary Science, Cosmic infrared background, galaxies: statistic, Surface brightness, galaxies: evolution, Order of magnitude, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The cosmic infrared background (CIB) includes roughly half of the energy radiated by all galaxies at all wavelengths across cosmic time, as observed at the present epoch. The PACS Evolutionary Probe (PEP) survey is exploited here to study the CIB and its redshift differential, at 70, 100 and 160 micron, where the background peaks. Combining PACS observations of the GOODS-S, GOODS-N, Lockman Hole and COSMOS areas, we define number counts spanning over more than two orders of magnitude in flux: from ~1 mJy to few hundreds mJy. Stacking of 24 micron sources and P(D) statistics extend the analysis down to ~0.2 mJy. Taking advantage of the wealth of ancillary data in PEP fields, differential number counts and CIB are studied up to z=5. Based on these counts, we discuss the effects of confusion on PACS blank field observations and provide confusion limits for the three bands considered. The total CIB surface brightness emitted above PEP 3 sigma flux limits is 4.52 +/- 1.18, 8.35 +/- 0.95 and 9.49 +/- 0.59 [nW/m2/sr] at 70, 100, and 160 micron, respectively. These values correspond to 58 +/- 7% and 74 +/- 5% of the COBE/DIRBE CIB direct measurements at 100 and 160 micron. Employing the P(D) analysis, these fractions increase to ~65% and ~89%. More than half of the resolved CIB was emitted at redshift z1.0 sources reaches 50% at 160 micron. Most of the CIB resolved in the three PACS bands was emitted by galaxies with infrared luminosities in the range 1e11-1e12 L(sun)., Proposed for acceptance on A&A

Published
2011

20. Herschel unveils a puzzling uniformity of distant dusty galaxies

Author

D. Elbaz, H. S. Hwang, B. Magnelli, E. Daddi, H. Aussel, B. Altieri, A. Amblard, P. Andreani, V. Arumugam, R. Auld, T. Babbedge, S. Berta, A. Blain, J. Bock, A. Bongiovanni, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodriguez, A. Cava, J. Cepa, P. Chanial, R.-R. Chary, A. Cimatti, D. L. Clements, A. Conley, L. Conversi, A. Cooray, M. Dickinson, H. Dominguez, C. D. Dowell, J. S. Dunlop, E. Dwek, S. Eales, D. Farrah, N. Förster Schreiber, M. Fox, A. Franceschini, W. Gear, R. Genzel, J. Glenn, M. Griffin, C. Gruppioni, M. Halpern, E. Hatziminaoglou, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, D. Le Borgne, E. Le Floc'h, L. Levenson, N. Lu, D. Lutz, S. Madden, B. Maffei, G. Magdis, G. Mainetti, R. Maiolino, L. Marchetti, A. M. J. Mortier, H. T. Nguyen, R. Nordon, B. O'Halloran, K. Okumura, S. J. Oliver, A. Omont, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Perez Fournon, A. M. Pérez García, A. Poglitsch, M. Pohlen, P. Popesso, F. Pozzi, J. I. Rawlings, D. Rigopoulou, L. Riguccini, D. Rizzo, G. Rodighiero, I. G. Roseboom, M. Rowan-Robinson, A. Saintonge, M. Sanchez Portal, P. Santini, M. Sauvage, B. Schulz, D. Scott, N. Seymour, L. Shao, D. L. Shupe, A. J. Smith, J. A. Stevens, E. Sturm, M. Symeonidis, L. Tacconi, M. Trichas, K. E. Tugwell, M. Vaccari, I. Valtchanov, J. Vieira, L. Vigroux, L. Wang, R. Ward, G. Wright, C. K. Xu, M. Zemcov, Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-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), Elbaz D., Hwang H. S., Magnelli B., Daddi E., Aussel H., Altieri B., Amblard A., Andreani P., Arumugam V., Auld R., Babbedge T., Berta S., Blain A., Bock J., Bongiovanni A., Boselli A., Buat V., Burgarella D., Castro-Rodriguez N., Cava A., Cepa J., Chanial P., Chary R.-R., Cimatti A., Clements D. L., Conley A., Conversi L., Cooray A., Dickinson M., Dominguez H., Dowell C. D., Dunlop J. S., Dwek E., Eales S., Farrah D., Förster Schreiber N., Fox M., Franceschini A., Gear W., Genzel R., Glenn J., Griffin M., Gruppioni C., Halpern M., Hatziminaoglou E., Ibar E., Isaak K., Ivison R. J., Lagache G., Le Borgne D., Le Floc'h E., Levenson L., Lu N., Lutz D., Madden S., Maffei B., Magdis G., Mainetti G., Maiolino R., Marchetti L., Mortier A. M. J., Nguyen H. T., Nordon R., O'Halloran B., Okumura K., Oliver S. J., Omont A., Page M. J., Panuzzo P., Papageorgiou A., Pearson C. P., Perez Fournon I., Pérez García A. M., Poglitsch A., Pohlen M., Popesso P., Pozzi F., Rawlings J. I., Rigopoulou D., Riguccini L., Rizzo D., Rodighiero G., Roseboom I. G., Rowan-Robinson M., Saintonge A., Sanchez Portal M., Santini P., Sauvage M., Schulz B., Scott D., Seymour N., Shao L., Shupe D. L., Smith A. J., Stevens J. A., Sturm E., Symeonidis M., Tacconi L., Trichas M., Tugwell K. E., Vaccari M., Valtchanov I., Vieira J., Vigroux L., Wang L., Ward R., Wright G., Xu C. K., and Zemcov M.

Subjects
Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, infrared: galaxies, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Bolometer, Astronomy and Astrophysics, Redshift, Space observatory, Galaxy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved since z~2.5. We use Herschel deep extragalactic surveys from 100 to 500um to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and HerMES key programs). We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used to identify isolated galaxies whose flux is not boosted by bright neighbors. Below z~1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15dex), therefore similar to z~0 galaxies. This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160um, 250um or 350um bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ~150um (rest-frame) on local templates. We also note that the dust temperature of luminous IR galaxies around z~1 is mildly colder by 10-15% than their local analogs and up to 20% for ULIRGs at z~1.6. Above z=1.5, distant galaxies are found to exhibit a substantially larger mid- over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor star formation at very high SFR and in conditions similar to purely star-forming galaxies., Astronomy and Astrophysics, Herschel Special Issue, in press as a Letter; 5 pages

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