GOODS–Herschel: an infrared main sequence for star-forming galaxies
David Elbaz,Mark Dickinson,Ho Seong Hwang,Tanio Díaz-Santos,Georgios E. Magdis,Benjamin Magnelli,D. Le Borgne,Frédéric Galliano,Maurilio Pannella,P. Chanial,Lee Armus,Vassilis Charmandaris,Vassilis Charmandaris,Emanuele Daddi,Herve Aussel,P. Popesso,Jeyhan S. Kartaltepe,Bruno Altieri,Ivan Valtchanov,D. Coia,Helmut Dannerbauer,Kalliopi Dasyra,Roger Leiton,Roger Leiton,Joseph M. Mazzarella,David M. Alexander,V. Buat,Denis Burgarella,R.-R. Chary,Roberto Gilli,Rob Ivison,Rob Ivison,Stéphanie Juneau,E. Le Floc'h,Dieter Lutz,G. E. Morrison,James Mullaney,Eric J. Murphy,Alexandra Pope,Douglas Scott,Mark Brodwin,Daniela Calzetti,C. Cesarsky,Stéphane Charlot,Herve Dole,Peter Eisenhardt,Henry C. Ferguson,N. M. Förster Schreiber,Dave Frayer,Mauro Giavalisco,Minh Huynh,Anton M. Koekemoer,Casey Papovich,Naveen A. Reddy,Christian Surace,Harry I. Teplitz,Min S. Yun,G. W. Wilson +57 more
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In this paper, the authors examined the infrared (IR) 3-500μm spectral energy distributions (SEDs) of galaxies at 0 < z < 2.5, supplemented by a local reference sample from IRAS, ISO, Spitzer, and AKARI data.Abstract:
We present the deepest 100 to 500 μm far-infrared observations obtained with the Herschel Space Observatory as part of the GOODS-Herschel key program, and examine the infrared (IR) 3–500 μm spectral energy distributions (SEDs) of galaxies at 0 < z < 2.5, supplemented by a local reference sample from IRAS, ISO, Spitzer, and AKARI data. We determine the projected star formation densities of local galaxies from their radio and mid-IR continuum sizes.
We find that the ratio of total IR luminosity to rest-frame 8 μm luminosity, IR8 (≡ L_(IR)^(tot)/L_8), follows a Gaussian distribution centered on IR8 = 4 (σ = 1.6) and defines an IR main sequence for star-forming galaxies independent of redshift and luminosity. Outliers from this main sequence produce a tail skewed toward higher values of IR8. This minority population ( 3 × 10^(10) L_⊙ kpc^(-2)) and a high specific star formation rate (i.e., starbursts). The rest-frame, UV-2700 A size of these distant starbursts is typically half that of main sequence galaxies, supporting the correlation between star formation density and starburst activity that is measured for the local sample.
Locally, luminous and ultraluminous IR galaxies, (U)LIRGs (L_(IR)^(tot)≥ 10^(11) L_☉), are systematically in the starburst mode, whereas most distant (U)LIRGs form stars in the “normal” main sequence mode. This confusion between two modes of star formation is the cause of the so-called “mid-IR excess” population of galaxies found at z > 1.5 by previous studies. Main sequence galaxies have strong polycyclic aromatic hydrocarbon (PAH) emission line features, a broad far-IR bump resulting from a combination of dust temperatures (T_(dust) ~ 15–50 K), and an effective T_(dust) ~ 31 K, as derived from the peak wavelength of their infrared SED. Galaxies in the starburst regime instead exhibit weak PAH equivalent widths and a sharper far-IR bump with an effective T_(dust)~ 40 K. Finally, we present evidence that the mid-to-far IR emission of X-ray active galactic nuclei (AGN) is predominantly produced by star formation and that candidate dusty AGNs with a power-law emission in the mid-IR systematically occur in compact, dusty starbursts. After correcting for the effect of starbursts on IR8, we identify new candidates for extremely obscured AGNs.read more
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The molecular gas content in obscured AGN at z > 1.
Michele Perna,Mark Sargent,Marcella Brusa,Emanuele Daddi,Chiara Feruglio,Giovanni Cresci,Giorgio Lanzuisi,Elisabeta Lusso,Andrea Comastri,R. T. Coogan,Q. D'Amato,Roberto Gilli,Enrico Piconcelli,C. Vignali +13 more
TL;DR: In this article, the authors measured the cold gas reservoir of three highly obscured QSOs to test if their gas fraction is similar to that of sub-millimeter galaxies (SMGs), as expected by some models, and place these measurements in the context of the SB-QSO framework.
Journal ArticleDOI
Integral Field Spectroscopy based H\alpha\ sizes of local Luminous and Ultraluminous Infrared Galaxies. A Direct Comparison with high-z Massive Star Forming Galaxies
Santiago Arribas,Luis Colina,A. Alonso-Herrero,F. F. Rosales-Ortega,Ana Monreal-Ibero,M. Garcia-Marin,Santiago García-Burillo,J. Rodriguez-Zaurin +7 more
TL;DR: In this article, the authors compare the similarities between local U/LIRGs and high-z massive SFGs by comparing basic Hα structural characteristics, such as size, and luminosity (and SFR) surface density, in an homogeneous way.
Journal ArticleDOI
The host galaxies of x-ray quasars are not strong star formers* ** *** **** *****
Amy J. Barger,Amy J. Barger,Lennox L. Cowie,Frazer N. Owen,Chian-Chou Chen,Guenther Hasinger,Li-Yen Hsu,Yanxia Li +7 more
TL;DR: In this article, the authors measured the sub-millimeter fluxes of the 4-8 keV sources at the highest X-ray luminosities and found that most of the host galaxies are not strong star formers, perhaps because their star formation is suppressed by AGN feedback.
Journal ArticleDOI
Dust-obscured star formation in the outskirts of XMMU J2235.3−2557, a massive galaxy cluster at z = 1.4
J. S. Santos,Bruno Altieri,P. Popesso,V. Strazzullo,I. Valtchanov,S. Berta,Hans Böhringer,Luca Conversi,R. Demarco,Alastair C. Edge,C. Lidman,Dieter Lutz,L. Metcalfe,C. R. Mullis,I. Pintos-Castro,I. Pintos-Castro,M. Sánchez-Portal,T. D. Rawle,Piero Rosati,A. M. Swinbank,Masayuki Tanaka +20 more
TL;DR: In this article, the spectral energy distribution (SED) of XMMU J2235.3−2557 was used to detect star formation in a few z > 1.4 clusters.
Journal ArticleDOI
Measuring Star Formation Rate and Far-infrared Color in High-redshift Galaxies Using the CO(7–6) and [N II] 205 μm Lines
Nanyao Lu,Yinghe Zhao,Yinghe Zhao,C. Kevin Xu,Yu Gao,Tanio Díaz-Santos,Tanio Díaz-Santos,Vassilis Charmandaris,Hanae Inami,Justin Howell,Lijie Liu,Lijie Liu,Lee Armus,Joseph M. Mazzarella,George C. Privon,Steven D. Lord,David B. Sanders,Bernhard Schulz,Paul van der Werf +18 more
TL;DR: In this paper, the authors exploit a new spectroscopic approach involving only two emission lines: CO(7-6) at 372 μm and [N ii] at 205 μm.
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