The Main Sequence at z ∼ 1.3 Contains a Sizable Fraction of Galaxies with Compact Star Formation Sizes: A New Population of Early Post-starbursts?

Puglisi, A.; Daddi, E.; Liu, D.; Bournaud, F.; Silverman, John D.; Circosta, C.; Calabró, Antonello; Aravena, M.; Cibinel, A.; Dannerbauer, H.; Delvecchio, I.; Elbaz, D.; Gao, Yu; Gobat, R.; Jin, S.; Floc’h, E. Le; Magdis, G.; Mancini, C.; Riechers, Dominik A.; Rodighiero, G.; Sargent, M.; Valentino, F.; Zanisi, Lorenzo

doi:10.3847/2041-8213/ab1f92

Cited by 78 publications

(145 citation statements)

References 55 publications

Supporting

Mentioning

110

Contrasting

Order By: Relevance

“…A.1 and A.2) also suggests the presence of compact or clumpy optical morphologies, which seem to be common in distant starforming and Herschel-selected galaxies. Consistent with these results, using ALMA observations Puglisi et al (2019) recently found that a significant fraction, that is, ∼50%, of their sample comprising 93 Herschel-selected galaxies at 1.1 ≤ z ≤ 1.7 and at the MS show a compact morphology. The authors interpret their sources as early post-starburst galaxies.…”

Section: Star Formation Enhancement and Gas Enrichmentsupporting

confidence: 62%

Molecular gas and star formation activity in luminous infrared galaxies in clusters at intermediate redshifts

Castignani

Jablonka

Combes

et al. 2020

A&A

View full text Add to dashboard Cite

We investigate the role of dense megaparsec-scale environments in processing molecular gas of cluster galaxies as they fall into the cluster cores. We selected a sample of ∼20 luminous infrared galaxies (LIRGs) belonging to intermediate-redshift clusters, mainly from the Herschel Lensing Survey and the Local Cluster Substructure Survey. These galaxies include MACS J0717.5+3745 at z = 0.546 and Abell 697, 963, 1763, and 2219 at z = 0.2 − 0.3. We performed spectral energy distribution modeling from the far-infrared to ultraviolet of the LIRGs, which span cluster-centric distances within r/r200 ≃ 0.2 − 1.6. We observed the LIRGs in CO(1→0) or CO(2→1) with the Plateau de Bure interferometer and its successor NOEMA, as part of five observational programs carried out between 2012 and 2017. We compared the molecular gas to stellar mass ratio M(H2)/M⋆, star formation rate (SFR), and depletion time (τdep) of the LIRGs with those of a compilation of cluster and field star-forming galaxies from the literature. The targeted LIRGs have SFR, M(H2)/M⋆, and τdep that are consistent with those of both main-sequence (MS) field galaxies and star-forming galaxies from the comparison sample. However we find that the depletion time, normalized to the MS value, tentatively increases with increasing r/r200, with a significance of 2.8σ, which is ultimately due to a deficit of cluster-core LIRGs with τdep ≳ τdep, MS. We suggest that a rapid exhaustion of the molecular gas reservoirs occurs in the cluster LIRGs and is indeed effective in suppressing their star formation and ultimately quenching them. This mechanism may explain the exponential decrease of the fraction of cluster LIRGs with cosmic time. The compression of the gas in LIRGs, possibly induced by intra-cluster medium shocks, may be responsible for the short timescales that are observed in a large fraction of cluster-core LIRGs. Some of our LIRGs may also belong to a population of infalling filament galaxies.

show abstract

Section: Star Formation Enhancement and Gas Enrichmentsupporting

confidence: 62%

Molecular gas and star formation activity in luminous infrared galaxies in clusters at intermediate redshifts

Castignani

Jablonka

Combes

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…Di Matteo et al 2008;Hung et al 2013;Cibinel et al 2019), demonstrate that merging systems may lie on the main sequence. Puglisi et al (2019) find that up to 50% of the most massive galaxies on the MS at z ∼ 1.3 may have star formation driven by merging. Major merger activity may not enhance star formation rates at every stage of a merger (e.g.…”

Section: Main Sequence Of Galaxiesmentioning

confidence: 90%

Three Dusty Star-forming Galaxies at z ∼ 1.5: Mergers and Disks on the Main Sequence

Drew

Casey

Cooray

et al. 2020

ApJ

View full text Add to dashboard Cite

The main sequence of galaxies, a correlation between the star formation rates and stellar masses of galaxies, has been observed out to z ∼ 4. Galaxies within the scatter of the correlation are typically interpreted to be secularly evolving while galaxies with star formation rates elevated above the main sequence are interpreted to be undergoing interactions or to be Toomre-unstable disks with starbursting clumps. In this paper we investigate the recent merger histories of three dusty star forming galaxies, identified by their bright submillimeter emission at z ∼ 1.5. We analyze rest-frame optical and UV imaging, rest-frame optical emission line kinematics using slit spectra obtained with MOSFIRE on Keck I, and calculate Gini and M 20 statistics for each galaxy and conclude two are merger-driven while the third is an isolated disk galaxy. The disk galaxy lies ∼4× above the main sequence, one merger lies within the scatter of the main sequence, and one merger lies ∼4× below the main sequence. This hints that the location of a galaxy with respect to the main sequence may not be a useful discriminator of the recent star formation history of high-M galaxies at z ∼ 1.

show abstract

“…Part of the data has been already used in previous works. In particular, Puglisi et al (2019) focused on the far-IR sizes of our sample and anticipated the blurred difference between upper MS and SB galaxies mentioned above, revealing a significant population of post-starburst galaxies on the main sequence. A more articulated analysis of the role of compactness on galaxy evolution is in preparation (Puglisi et al, in prep.).…”

Section: Introductionmentioning

confidence: 97%

“…The same definition of starbursts as galaxies deviating from the main sequence has been recently questioned with the advent of high spatial resolution measurements of their dust and gas emission. Compact galaxies with short depletion timescales typical of SBs are now routinely found on the MS, being possibly on their way to leave the sequence (Barro et al 2017a;Popping et al 2017;Elbaz et al 2018;Gómez-Guijarro et al 2019;Puglisi et al 2019;Jiménez-Andrade et al 2019); or galaxies moving within the MS scatter, due to mergers unable to efficiently boost the star formation (Fensch et al 2017) or owing to gravitational instabilities and gas radial redistribution (Tacchella et al 2016).…”

Section: Introductionmentioning

confidence: 99%

CO emission in distant galaxies on and above the main sequence

Valentino

Daddi

Puglisi

et al. 2020

A&A

Self Cite

View full text Add to dashboard Cite

We present the detection of multiple carbon monoxide CO line transitions with ALMA in a few tens of infrared-selected galaxies on and above the main sequence at z = 1.1−1.7. We reliably detected the emission of CO (5 − 4), CO (2 − 1), and CO (7 − 6)+[C I](3P2 − 3P1) in 50, 33, and 13 galaxies, respectively, and we complemented this information with available CO (4 − 3) and [C I](3P1 − 3P0) fluxes for part of the sample, and by modeling of the optical-to-millimeter spectral energy distribution. We retrieve a quasi-linear relation between LIR and CO (5 − 4) or CO (7 − 6) for main-sequence galaxies and starbursts, corroborating the hypothesis that these transitions can be used as star formation rate (SFR) tracers. We find the CO excitation to steadily increase as a function of the star formation efficiency, the mean intensity of the radiation field warming the dust (⟨U⟩), the surface density of SFR (ΣSFR), and, less distinctly, with the distance from the main sequence (ΔMS). This adds to the tentative evidence for higher excitation of the CO+[C I] spectral line energy distribution (SLED) of starburst galaxies relative to that for main-sequence objects, where the dust opacities play a minor role in shaping the high-J CO transitions in our sample. However, the distinction between the average SLED of upper main-sequence and starburst galaxies is blurred, driven by a wide variety of intrinsic shapes. Large velocity gradient radiative transfer modeling demonstrates the existence of a highly excited component that elevates the CO SLED of high-redshift main-sequence and starbursting galaxies above the typical values observed in the disk of the Milky Way. This excited component is dense and it encloses ∼50% of the total molecular gas mass in main-sequence objects. We interpret the observed trends involving the CO excitation as to be mainly determined by a combination of large SFRs and compact sizes, as a large ΣSFR is naturally connected with enhanced dense molecular gas fractions and higher dust and gas temperatures, due to increasing ultraviolet radiation fields, cosmic ray rates, as well as dust and gas coupling. We release the full data compilation and the ancillary information to the community.

show abstract

The Main Sequence at z ∼ 1.3 Contains a Sizable Fraction of Galaxies with Compact Star Formation Sizes: A New Population of Early Post-starbursts?

Cited by 78 publications

References 55 publications

Molecular gas and star formation activity in luminous infrared galaxies in clusters at intermediate redshifts

Molecular gas and star formation activity in luminous infrared galaxies in clusters at intermediate redshifts

Three Dusty Star-forming Galaxies at z ∼ 1.5: Mergers and Disks on the Main Sequence

CO emission in distant galaxies on and above the main sequence

Contact Info

Product

Resources

About