Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift

Scoville, N. Z.; Lee, N.; Bout, P. A. Vanden; Díaz-Santos, T.; Sanders, D. B.; Darvish, Behnam; Bongiorno, A.; Casey, Caitlin M.; Murchikova, Lena; Koda, Jin; Capak, P.; Vlahakis, C.; Ilbert, O.; Sheth, Kartik; Morokuma-Matsui, Kana; Ivison, R. J.; Aussel, H.; Laigle, C.; McCracken, H. J.; Armus, L.; Pope, Alexandra; Toft, Sune; Masters, D. C.

doi:10.3847/1538-4357/aa61a0

Cited by 377 publications

(744 citation statements)

References 79 publications

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“…We note that we reach a similar conclusion when we consider a weaker dependance of f gas on sS FR/sS FR MS (γ ≈ 0.3 − 0.6) reported by other studies (e.g. Genzel et al 2015, Scoville et al 2017, Tacconi et al 2017.…”

Section: Star Formation Law and Sfe Of Z = 3 Ms Galaxiessupporting

confidence: 90%

“…While whether (a) SBs deviate from the L IR −L ′ CO relation of MS galaxies as a power-law to their offset from the MS (e.g. Tacconi et al 2017, Scoville et al 2017 there is a more abrupt transition between the MS and SB regime (2-SFM paradigm, Sargent et al 2014), is still an open question, it is clear that SB galaxies have systematically larger…”

Section: Star Formation Law and Sfe Of Z = 3 Ms Galaxiesmentioning

confidence: 99%

“…ms to the MS, (sS FR/sS FR MS ) γ (e.g. Magdis et al 2012b, Sargent et al 2014, Genzel et al 2015, Scoville et al 2017. Adopting γ = 0.8 from Magdis et al (2012b) and taking into account that D49 and M28 lie ×1.5 and ×1.4 above and below the MS respectively, suggests ∼ ×2 higher f gas in D49 compared to M28.…”

Section: Star Formation Law and Sfe Of Z = 3 Ms Galaxiesmentioning

confidence: 99%

“…Also, Scoville et al (2017) and Schinnerer et al (2016), were able to place constraints on the gas masses of individual galaxies up to z = 4, using single band measurements of the dust emission flux on the Rayleigh-Jeans side of their SED. Finally, Magdis et al (2012a), and Tan et al (2014), presented CO observations, and therefore M H 2 estimates for a couple of z = 3 − 4 Lyman Break Galaxies (LBGs).…”

Section: Introductionmentioning

confidence: 99%

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Dust and gas in star-forming galaxies at z ~ 3

Magdis¹,

Rigopoulou²,

Daddi³

et al. 2017

A&A

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We present millimetre dust emission measurements of two Lyman Break Galaxies at z ∼ 3 and construct for the first time fully sampled infrared spectral energy distributions (SEDs), from mid-IR to the Rayleigh-Jeans tail, of individually detected, unlensed, UV-selected, main sequence (MS) galaxies at z = 3. The SED modelling of the two sources confirms previous findings, based on stacked ensembles, of an increasing mean radiation field U with redshift, consistent with a rapidly decreasing gas metallicity in z > 2 galaxies. Complementing our study with CO[J=3→2] emission line observations, we measure the molecular gas mass reservoir (M H 2 ) of the systems using three independent approaches: 1) CO line observations, 2) the dust to gas mass ratio vs metallicity relation and 3) a single band, dust emission flux on the Rayleigh-Jeans side of the SED. All techniques return consistent M H 2 estimates within a factor of ∼2 or less, yielding gas depletion time-scales (τ dep ≈ 0.35 Gyrs) and gas-to-stellar mass ratios (M H 2 /M * ≈ 0.5 − 1) for our z ∼ 3 massive MS galaxies. The overall properties of our galaxies are consistent with trends and relations established at lower redshifts, extending the apparent uniformity of star forming-galaxies over the last 11.5 billion years.

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Section: Star Formation Law and Sfe Of Z = 3 Ms Galaxiessupporting

confidence: 90%

Section: Star Formation Law and Sfe Of Z = 3 Ms Galaxiesmentioning

confidence: 99%

Section: Star Formation Law and Sfe Of Z = 3 Ms Galaxiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Dust and gas in star-forming galaxies at z ~ 3

Magdis¹,

Rigopoulou²,

Daddi³

et al. 2017

A&A

Self Cite

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show abstract

“…The interplay between these has been encapsulated in so-called 'scaling relations' in several recent studies referring to large, statistical samples (e.g. Santini et al 2014;Sargent et al 2014;Genzel et al 2015;Scoville et al 2017;Tacconi et al 2017). Similarly, cosmological simulations and semi-analytical models have started to predict the relative importance of molecular gas as a function of redshift, and find that the role of H 2 in galaxies becomes increasingly dominant at higher redshifts (e.g.…”

Section: Introductionmentioning

confidence: 99%

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

Coogan

Daddi

Sargent

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We use ALMA and JVLA observations of the galaxy cluster Cl J1449+0856 at z=1.99, in order to study how dust-obscured star-formation, ISM content and AGN activity are linked to environment and galaxy interactions during the crucial phase of high-z cluster assembly. We present detections of multiple transitions of 12 CO, as well as dust continuum emission detections from 11 galaxies in the core of Cl J1449+0856. We measure the gas excitation properties, star-formation rates, gas consumption timescales and gas-to-stellar mass ratios for the galaxies.We find evidence for a large fraction of galaxies with highly-excited molecular gas, contributing >50% to the total SFR in the cluster core. We compare these results with expectations for field galaxies, and conclude that environmental influences have strongly enhanced the fraction of excited galaxies in this cluster. We find a dearth of molecular gas in the galaxies' gas reservoirs, implying a high star-formation efficiency (SFE) in the cluster core, and find short gas depletion timescales τ<0.1-0.4 Gyrs for all galaxies. Interestingly, we do not see evidence for increased specific star-formation rates (sSFRs) in the cluster galaxies, despite their high SFEs and gas excitations. We find evidence for a large number of mergers in the cluster core, contributing a large fraction of the core's total star-formation compared with expectations in the field. We conclude that the environmental impact on the galaxy excitations is linked to the high rate of galaxy mergers, interactions and active galactic nuclei in the cluster core.

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Molecular gas in distant galaxies from ALMA studies

Combes

2018

Astron Astrophys Rev

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ALMA is now fully operational, and has been observing in early science mode since 2011. The millimetric (mm) and sub-mm domain is ideal to tackle galaxies at high redshift, since the emission peak of the dust at 100µm is shifted in the ALMA bands (0.3mm to 1mm) for z=2 to 9, and the CO lines, stronger at the high-J levels of the ladder, are found all over the 0.3-3mm range. Pointed surveys and blind deep fields have been observed, and the wealth of data collected reveal a drop at high redshifts (z > 6) of dusty massive objects, although surprisingly active and gas-rich objects have been unveiled through gravitational lensing. The window of the reionization epoch is now wide open, and ALMA has detected galaxies at z=8-9 mainly in continuum, [CII] and [OIII] lines. Galaxies have a gas fraction increasing steeply with redshift, as (1+z) 2 , while their star formation efficiency increases also but more slightly, as (1+z) 0.6 to (1+z) 1 . Individual object studies have revealed luminous quasars, with black hole masses much higher than expected, clumpy galaxies with resolved star formation rate compatible with the Kennicutt-Schmidt relation, extended cold and dense gas in a circumgalactic medium, corresponding to Lyman-α blobs, and proto-clusters, traced by their brightest central galaxies.

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Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift

Cited by 377 publications

References 79 publications

Dust and gas in star-forming galaxies at z ~ 3

Dust and gas in star-forming galaxies at z ~ 3

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

Molecular gas in distant galaxies from ALMA studies

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