Cool Gas in High-Redshift Galaxies

By C. Carilli, F. Walter. 2013

838 citations recorded by the source corpus.

Over the past decade, observations of the cool interstellar medium (ISM) in distant galaxies via molecular and atomic fine structure line (FSL) emission have gone from a curious look into a few extreme, rare objects to a mainstream tool for studying galaxy formation out to the highest redshifts. Molecular gas has been observed in close to 200 galaxies at z > 1, including numerous AGN host-galaxies out to z ∼ 7, highly star-forming submillimeter galaxies, and increasing samples of main-sequence color-selected star-forming galaxies at z ∼ 1.5 to 2.5. Studies have moved well beyond simple detections to dynamical imaging at kiloparsec-scale resolution and multiline, multispecies studies that determine the physical conditions in the ISM in early galaxies. Observations of the cool gas are the required complement to studies of the stellar density and star-formation history of the Universe as they reveal the phase of the ISM that immediately precedes star formation in galaxies. Current observations suggest that t...

Subfields: Astronomy and Astrophysics, Instrumentation

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KILOPARSEC-SCALE DUST DISKS IN HIGH-REDSHIFT LUMINOUS SUBMILLIMETER GALAXIES (2016, background): “However, such studies have been very expensive observationally, and in many cases at best marginally resolve the sources (see Carilli & Walter 2013 for a review).”
The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, background): “…evolution of the gas and dust content (e.g. Tacconi et al. 2013; Santini et al. 2014; Bothwell et al. 2013; Genzel et al. 2010; Daddi et al. 2010; Carilli & Walter 2013), to investigate their dynamics (e.g. Wang et al. 2013; De Breuck et al. 2014; Carniani et al. 2013; Carilli et al. 2013;…”
Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, methodology): “…the line luminosity, we use the following rela- tion Lline =1.04×10 −3 × ( Sline∆v Jy km s−1 )( DL Mpc )2 ( νobs GHz ) L⊙(1) 3 http://www.cv.nrao.edu/php/splat/ (Carilli & Walter 2013), where Sline∆v is the velocityintegrated flux, DL is the luminosity distance, and νobs is the observed frequency.”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “This much more rapid quenching in high redshift clusters could be due to the shorter gas consumption timescales of galaxies at z ∼ 1 (Carilli & Walter 2013) or ∼1.7× shorter cluster crossing timescales.”
COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, background): “…in z>0.5 galaxies were restricted to luminous, gas and dust rich, outliers, such as starbursts and mergers, significantly above the main-sequence line at their respective redshifts (e.g. Greve et al. 2005, Tacconi et al. 2006, 2008, Riechers 2013, Carilli & Walter 2013, Bothwell et al. 2013).”
The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, methodology): “…galaxies have been made possible with facilities such as the Atacama Large Millimeter Array (ALMA), allowing for direct measurements of either the dust continuum or far-IR spectral features for more typical star-forming galaxies in the distant universe (Carilli & Walter 2013; Dunlop et al. 2017).”
CO excitation of normal star forming galaxies out to $z=1.5$ as regulated by the properties of their interstellar medium (2014, methodology): “Future observations will clarify whether CO[5-4] can be used as a more eff ctive (i.e. less time–consuming) alternative to HCN to study the dense SF gas in galaxies.”
THE EVOLUTION OF INTERSTELLAR MEDIUM MASS PROBED BY DUST EMISSION: ALMA OBSERVATIONS AT z = 0.3–2 (2014, background): “Following the peak in cosmic star formation (SF) at z = 2.5, the overall star formation rate has declined by a factor of 20 over the last 11 Gyr (Hopkins & Beacom 2006; Carilli & Walter 2013).”
Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift (2017, methodology): “…(Tacconi et al. 2010; Daddi et al. 2010; Genzel et al. 2010; Riechers et al. 2011; Ivison et al. 2011; Magdis et al. 2012b; Saintonge et al. 2013; Carilli & Walter 2013; Tacconi et al. 2013; Bolatto et al. 2015; Genzel et al. 2015), the sample of galaxies used here has the virtue that it maps…”
Physical Properties of 15 Quasars at z ≳ 6.5 (2017, methodology): “We can also calculate the luminosity of the [CII] emission line (L[CII]) from the observed line flux (S[CII]∆v; Carilli & Walter 2013): L[CII] L = 1.04× 10−3 S[CII]∆v Jy km s−1 ( DL Mpc )2 νobs GHz (15) where DL is the luminosity distance and νobs is the observed frequency.”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “First, a new generation of sub-mm and radio interferometers (including ALMA, NOEMA, JVLA, Apertif, ASKAP, MeerKAT, and the SKA) will literally revolutionize our ability to characterize the cold gas in the ISM of galaxies out to high redshifts (Carilli & Walter 2013).”
Dusty Star Forming Galaxies at High Redshift (2014, background): “A summary of critical densities for a number of commonly observed molecular and atomic line transitions is given in Carilli and Walter (2013) for T = 100 K. Oftentimes it is assumed that if a line is observed, the densities present in the emitting gas are above the critical density for the line…”
Very extended cold gas, star formation and outflows in the halo of a bright QSO at z>6 (2014, background): “…multi-wavelength studies, aimed at constraining the extreme properties of its host galaxy and of its cosmological environment (e.g. Bertoldi et al. 2003; Walter et al. 2003, 2004; Willott et al. 2003; Riechers et al. 2009; Gallerani et al. 2010; Decarli et al. 2012; Carilli & Walter 2013).”
THE FINAL SDSS HIGH-REDSHIFT QUASAR SAMPLE OF 52 QUASARS AT z > 5.7 (2016, background): “…rich information about dust emission and star formation in the host galaxies (e.g., Jiang et al. 2006, 2010; Walter et al. 2009; Gallerani et al. 2010; Wang et al. 2011, 2013; Carilli & Walter 2013; Omont et al. 2013; Calura et al. 2014; Leipski et al. 2014; Bañados et al. 2015; Lyu et al. 2016).”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, background): “…km s GHz Mpc , 1C 3 line 1 obs L 2 II where Fline is the integrated line flux (from the 2D fit of the line described in Section 4.2, corrected for the flux loss due to the line wings), nobs is the observed frequency of the line, and DL is the luminosity distance (see, e.g., Carilli & Walter 2013).”
ALMA IMAGING OF GAS AND DUST IN A GALAXY PROTOCLUSTER AT REDSHIFT 5.3: [C ii] EMISSION IN “TYPICAL” GALAXIES AND DUSTY STARBURSTS ≈1 BILLION YEARS AFTER THE BIG BANG (2014, methodology): “Derivation of Further Galaxy Properties We derive line luminosities from the observed [CII] intensities using standard relations (e.g., Solomon & vanden Bout 2005; Carilli & Walter 2013).”