The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

Eckert, K.; Kannappan, Sheila J.; Lagos, Claudia del P.; Baker, Ashley; Berlind, Andreas A.; Stark, David V.; Moffett, Amanda J.; Nasipak, Zachary; Norris, Mark A.

doi:10.3847/1538-4357/aa8e97

Cited by 14 publications

(15 citation statements)

References 106 publications

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“…The frequency of satellite galaxies decreases steadily with increasing stellar mass, while centrals display a double peaked distribution. This double-peaked distribution is connected to the efficiency of baryon collapse and star formation being maximal at stellar masses ≈ 10 10 M in both simulations and observations (Behroozi et al 2013;Eckert et al 2017).…”

Section: 2mentioning

confidence: 67%

“…The blue cloud is comparatively more dispersed, and is normally home to late-type galaxies with higher star formation rates (Baldry et al 2004;Driver et al 2006;Schiminovich et al 2007). Between these two populations is a region denoted the green valley, which appears in observations to be sparsely populated (Martin et al 2007;Salim 2014) (though work by Eales et al (2018) demonstrates that observational biases could be responsible for the under-density). Galaxy bimodal-ity can also be observed in SSFR-stellar mass space (Wyder et al 2007), where the blue cloud population in colour-mass space is correlated with the main sequence population in the SSFR-stellar mass plane (Noeske et al 2007;Davies et al 2016b).…”

Section: Introductionmentioning

confidence: 99%

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Quenching time-scales of galaxies in the eagle simulations

Wright

Lagos

Davies

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We use the eagle simulations to study the connection between the quenching timescale, τ Q , and the physical mechanisms that transform star-forming galaxies into passive galaxies. By quantifying τ Q in two complementary ways -as the time over which (i) galaxies traverse the green valley on the colour-mass diagram, or (ii) leave the main sequence of star formation and subsequently arrive on the passive cloud in specific star formation rate (SSFR)-mass space -we find that the τ Q distribution of high-mass centrals, low-mass centrals and satellites are divergent. In the low stellar mass regime where M < 10 9.6 M , centrals exhibit systematically longer quenching timescales than satellites (≈ 4 Gyr compared to ≈ 2 Gyr). Satellites with low stellar mass relative to their halo mass cause this disparity, with ram pressure stripping quenching these galaxies rapidly. Low mass centrals are quenched as a result of stellar feedback, associated with long τ Q 3 Gyr. At intermediate stellar masses where 10 9.7 M < M < 10 10.3 M , τ Q are the longest for both centrals and satellites, particularly for galaxies with higher gas fractions. At M 10 10.3 M , galaxy merger counts and black hole activity increase steeply for all galaxies. Quenching timescales for centrals and satellites decrease with stellar mass in this regime to τ Q 2 Gyr. In anticipation of new intermediate redshift observational galaxy surveys, we analyse the passive and star-forming fractions of galaxies across redshift, and find that the τ Q peak at intermediate stellar masses is responsible for a peak (inflection point) in the fraction of green valley central (satellite) galaxies at z ≈ 0.5 − 0.7.

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Section: 2mentioning

confidence: 67%

Section: Introductionmentioning

confidence: 99%

Quenching time-scales of galaxies in the eagle simulations

Wright

Lagos

Davies

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…For this work, we use the RESOLVE (REsolved Spectroscopy of a Local VolumE) survey, a volume-limited census of mass in stars, cold gas, and dark matter for a statistically complete subset of the z ∼ 0 galaxy population (Kannappan & Wei 2008;Eckert et al 2015Eckert et al , 2016Eckert et al , 2017Stark et al 2016). As a result of its volume-limited nature (see Figure 1), RESOLVE is ideal for examining the properties of the full low-z CDS population without the statistical completeness corrections necessary for flux-limited surveys.…”

Section: The Resolve Surveymentioning

confidence: 99%

“…The RESOLVE group catalog was defined by Eckert et al (2017) using the Friends-of-Friends (FoF) algorithm as described in Berlind et al (2006). The brightest galaxy in the r band in each group is labeled the central, and all other galaxies are labeled satellites.…”

Section: Full Survey Definition and Ancillary Datamentioning

confidence: 99%

Linking compact dwarf starburst galaxies in the RESOLVE survey to downsized blue nuggets

Palumbo

Kannappan

Frazer

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We identify and characterize compact dwarf starburst (CDS) galaxies in the RE-SOLVE survey, a volume-limited census of galaxies in the local universe, to probe whether this population contains any residual "blue nuggets," a class of intensely starforming compact galaxies first identified at high redshift z. Our 50 low-z CDS galaxies are defined by dwarf masses (stellar mass M * < 10 9.5 M ), compact bulged-disk or spheroid-dominated morphologies (using a quantitative criterion, µ ∆ > 8.6), and specific star formation rates above the defining threshold for high-z blue nuggets (log SSFR [Gyr −1 ] > −0.5). Across redshifts, blue nuggets exhibit three defining properties: compactness relative to contemporaneous galaxies, abundant cold gas, and formation via compaction in mergers or colliding streams. Those with halo mass below M halo ∼ 10 11.5 M may in theory evade permanent quenching and cyclically refuel until the present day. Selected only for compactness and starburst activity, our CDS galaxies generally have M halo 10 11.5 M and gas-to-stellar mass ratio 1. Moreover, analysis of archival DECaLS photometry and new 3D spectroscopic observations for CDS galaxies reveals a high rate of photometric and kinematic disturbances suggestive of dwarf mergers. The SSFRs, surface mass densities, and number counts of CDS galaxies are compatible with theoretical and observational expectations for redshift evolution in blue nuggets. We argue that CDS galaxies represent a maximally-starbursting subset of traditional compact dwarf classes such as blue compact dwarfs and blue E/S0s. We conclude that CDS galaxies represent a low-z tail of the blue nugget phenomenon formed via a moderated compaction channel that leaves open the possibility of disk regrowth and evolution into normal disk galaxies.

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“…Several empirical studies have inferred limits on the form of the HIHM relation. Eckert et al (2017) attempted to measure the "cold" baryon mass (stars plus ISM mass) vs. halo mass relation, for which they combined 21 cm-derived H masses with empirical estimates of the gas mass in galaxies based on the correlation between the H mass and optical colours in galaxies with detected H . The difficulty with this approach is the unknown systematic effects in the application of the empirical estimation to a wider parameter space than probed by actual H detections (see Eckert et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The physical drivers of the atomic hydrogen-halo mass relation

Chauhan,

Lagos,

Stevens

et al. 2020

Preprint

Self Cite

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We use the state-of-the-art semi-analytic galaxy formation model, S, to investigate the physical processes involved in dictating the shape, scatter and evolution of the H -halo mass relation at 0 ≤ z ≤ 2. We compare S with H clustering and spectral stacking of the H -halo mass relation derived from observations finding excellent agreement with the former and a deficiency of H in S at M halo ≈ 10 12−13 M in the latter, but otherwise great agreement below and above that mass threshold. In S , we find that the H mass increases with the halo mass up to a critical mass of ≈ 10 11.8 M ; between ≈ 10 11.8 M and 10 13 M , the scatter in the relation increases by 0.7 dex and the H mass decreases with the halo mass on average (till M halo ∼ 10 12.5 M , after which it starts increasing); at M halo 10 13 M , the H content continues to increase with increasing halo mass, as a result of the increasing H contribution from satellite galaxies. We find that the critical halo mass of ≈ 10 12 M is largely set by feedback from Active Galactic Nuclei (AGN), and the exact shape and scatter of the H -halo mass relation around that mass is extremely sensitive to how AGN feedback is modelled, with other physical processes (e.g. stellar feedback, star formation and gas stripping in satellites) playing a less significant role. We also determine the main secondary parameters responsible for the scatter of the H -halo mass relation, namely the halo spin parameter at M vir < 10 11.8 M , and the fractional contribution from substructure to the total halo mass (M sat h /M vir ) for M vir > 10 13 M . The scatter at 10 11.8 M < M vir < 10 13 M is best described by the black-hole-to-stellar mass ratio of the central galaxy, reflecting the relevance of AGN feedback. We present a numerical model to populate dark matter-only simulations with H at 0 ≤ z ≤ 2 based solely on halo parameters that are measurable in such simulations.

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The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

Cited by 14 publications

References 106 publications

Quenching time-scales of galaxies in the eagle simulations

Quenching time-scales of galaxies in the eagle simulations

Linking compact dwarf starburst galaxies in the RESOLVE survey to downsized blue nuggets

The physical drivers of the atomic hydrogen-halo mass relation

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