scholarly journals Ultra Massive Passive Galaxies at z~1.7

2015 ◽  
Vol 11 (S319) ◽  
pp. 111-111
Author(s):  
Liz Arcila-Osejo ◽  
Marcin Sawicki ◽  
Anneya Golob ◽  
Stephane Arnouts ◽  
Thibaud Moutard
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Effective Area ◽  
Dark Matter Halos ◽  
Quenching Mechanism ◽  
Massive Galaxies ◽  
Star Formation Activity ◽  
Stellar Masses ◽  
The Universe ◽  
Very High

AbstractAt redshift z~1.7 the Universe was at the peak of its star-formation activity. It is thus a puzzle why some galaxies, many of them very massive (M* ⩾ 1011 M⊙), had already chosen to stop forming stars. These ultra-massive galaxies, guaranteed to be the central galaxies of their host dark matter halos, must have attained very high rates of star formation to assemble their stellar masses in such a short amount of time. Using the largest (to date) K-selected gzKs survey of passive galaxies (in an effective area of ~ 27.5 deg2) we study the demographics of these dead monsters, hoping to help understand the quenching mechanism that shut them down.

scholarly journals Exhausted gas reservoirs drive massive galaxy quenching in the early universe

2020 ◽  
Author(s):  
Katherine Whitaker ◽  
Christina Williams ◽  
Lamiya Mowla ◽  
Justin Spilker ◽  
Sune Toft ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Gas ◽  
Dark Matter Halos ◽  
Gas Reservoirs ◽  
Massive Galaxies ◽  
Star Forming ◽  
Early Galaxies ◽  
Stellar Masses ◽  
Cold Dust ◽  
The Universe

Abstract When the Universe was merely three billion years old, about half of massive galaxies had already formed the bulk of their stars and new star formation plummeted [1]. How galaxies quench at such early times remains a puzzle, as their dark matter halos contain large gas reservoirs [2-4]. This gas should cool efficiently, sustaining star formation over long periods [5,6]. Here we present sensitive 1.3mm wavelength observations of cold dust in six quenched galaxies in the redshift range z=1.6 to z=3.2 with stellar masses ranging from 2.5x1010M⊙ to 5x1011M⊙, which are magnified by foreground galaxy clusters. Even with factors of up to 30 in magnification, four of the six galaxies are undetected at this wavelength. We show that these quenched galaxies have extremely little dust at early times, and by proxy very little cold molecular gas. The median dust mass is <0.01% of the stellar mass (molecular gas mass <1%), more than two orders of magnitude less than star-forming galaxies at this epoch [4]. The implication is that most early galaxies shut off star formation because their reservoir of molecular gas was rapidly depleted or removed, and is not being replenished.

scholarly journals The Slow Growth of Massive Galaxies in Rapidly Growing Dark Matter Halos

2009 ◽  
Vol 5 (S262) ◽  
pp. 244-247
Author(s):  
Michael J. I. Brown ◽  
Keyword(s):  
Dark Matter ◽  
Rapid Growth ◽  
Observational Studies ◽  
Cold Dark Matter ◽  
Slow Growth ◽  
Stellar Mass ◽  
Dark Matter Halos ◽  
Massive Galaxies ◽  
Stellar Masses ◽  
Red Galaxies

AbstractIn cold dark matter cosmologies, the most massive dark matter halos are predicted to undergo rapid growth at z < 1. While there is the expectation that massive galaxies will also rapidly grow via merging, recent observational studies conclude that the stellar masses of the most massive galaxies grow by just ~ 30% at z < 1. We have used the observed space density and clustering of z < 1 red galaxies in Boötes to determine how these galaxies populate dark matter halos. In the most massive dark matter halos, central galaxy stellar mass is proportional to halo mass to the power of a ~1/3 and much of the stellar mass resides within satellite galaxies. As a consequence, the most massive galaxies grow slowly even though they reside within rapidly growing dark matter halos.

scholarly journals A machine learning approach to measuring the quenched fraction of low-mass satellites beyond the Local Group

2021 ◽  
Author(s):  
Devontae C Baxter ◽  
M C Cooper ◽  
Sean P Fillingham
Keyword(s):  
Star Formation ◽  
Local Group ◽  
Local Environment ◽  
Sloan Digital Sky Survey ◽  
Data Sets ◽  
Quenching Mechanism ◽  
Star Formation Activity ◽  
Machine Learning Approach ◽  
Low Mass ◽  
Stellar Masses

Abstract Observations suggest that satellite quenching plays a major role in the build-up of passive, low-mass galaxies at late cosmic times. Studies of low-mass satellites, however, are limited by the ability to robustly characterize the local environment and star-formation activity of faint systems. In an effort to overcome the limitations of existing data sets, we utilize deep photometry in Stripe 82 of the Sloan Digital Sky Survey, in conjunction with a neural network classification scheme, to study the suppression of star formation in low-mass satellite galaxies in the local Universe. Using a statistically-driven approach, we are able to push beyond the limits of existing spectroscopic data sets, measuring the satellite quenched fraction down to satellite stellar masses of ∼107 M⊙ in group environments (Mhalo = 1013 − 14 h−1 M⊙). At high satellite stellar masses (≳ 1010 M⊙), our analysis successfully reproduces existing measurements of the quenched fraction based on spectroscopic samples. Pushing to lower masses, we find that the fraction of passive satellites increases, potentially signaling a change in the dominant quenching mechanism at M⋆ ∼ 109 M⊙. Similar to the results of previous studies of the Local Group, this increase in the quenched fraction at low satellite masses may correspond to an increase in the efficacy of ram-pressure stripping as a quenching mechanism in groups.

scholarly journals A Redshift-independent Efficiency Model: Star Formation and Stellar Masses in Dark Matter Halos at z ≳ 4

2018 ◽  
Vol 868 (2) ◽  
pp. 92 ◽  
Author(s):  
Sandro Tacchella ◽  
Sownak Bose ◽  
Charlie Conroy ◽  
Daniel J. Eisenstein ◽  
Benjamin D. Johnson
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Dark Matter Halos ◽  
Model Star ◽  
Stellar Masses

scholarly journals The chemical evolution of dwarf starburst galaxies

1999 ◽  
Vol 193 ◽  
pp. 679-691
Author(s):  
Francesca Matteucci ◽  
Annibale D'Ercole
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Chemical Evolution ◽  
Starburst Galaxies ◽  
Star Formation History ◽  
H Ii Regions ◽  
Dark Matter Halos ◽  
Star Formation Activity ◽  
Irregular Galaxies ◽  
Formation History

We will review the most popular models for the chemical evolution of some starburst galaxies, in particular dwarf irregular galaxies. These galaxies are relatively simple and unevolved objects with low metallicities and large gas contents, suggesting that they are either young or have undergone discontinuous star formation activity. Some dwarf irregulars are starburst galaxies currently experiencing an intense star formation event and they are known as blue compact galaxies or extragalactic H II regions. We will discuss the effects of the presence of dark matter halos together with stellar energetics (stellar winds and supernovae) on the development of a galactic wind in these systems. Particular emphasis will be given to the role of massive stars in driving the thermal and chemical evolution of the gas, in particular to type II supernovae. A comparison between different model predictions for abundances and abundance ratios will be used to impose constraints on the star formation history and on the amount of dark matter, which we found to be extremely important in these systems.

scholarly journals Exploring AGN and star formation activity of massive galaxies at cosmic noon

2020 ◽  
Vol 497 (3) ◽  
pp. 3273-3296
Author(s):  
Jonathan Florez ◽  
Shardha Jogee ◽  
Sydney Sherman ◽  
Matthew L Stevans ◽  
Steven L Finkelstein ◽  
...  
Keyword(s):  
Star Formation ◽  
Active Galactic Nucleus ◽  
Stellar Mass ◽  
Host Galaxies ◽  
X Ray ◽  
Massive Galaxies ◽  
Significant Time ◽  
Star Formation Activity ◽  
Quenching Process ◽  
Stellar Masses

ABSTRACT We investigate the relation between active galactic nucleus (AGN) and star formation (SF) activity at 0.5 &lt; z &lt; 3 by analysing 898 galaxies with X-ray luminous AGNs (LX &gt; 1044 erg s−1) and a large comparison sample of ∼320 000 galaxies without X-ray luminous AGNs. Our samples are selected from a large (11.8 deg2) area in Stripe 82 that has multiwavelength (X-ray to far-IR) data. The enormous comoving volume (∼0.3 Gpc3) at 0.5 &lt; z &lt; 3 minimizes the effects of cosmic variance and captures a large number of massive galaxies (∼30 000 galaxies with M* &gt; 1011 M⊙) and X-ray luminous AGNs. While many galaxy studies discard AGN hosts, we fit the SED of galaxies with and without X-ray luminous AGNs with Code Investigating GALaxy Emission and include AGN emission templates. We find that without this inclusion, stellar masses and star formation rates (SFRs) in AGN host galaxies can be overestimated, on average, by factors of up to ∼5 and ∼10, respectively. The average SFR of galaxies with X-ray luminous AGNs is higher by a factor of ∼3–10 compared to galaxies without X-ray luminous AGNs at fixed stellar mass and redshift, suggesting that high SFRs and high AGN X-ray luminosities may be fuelled by common mechanisms. The vast majority ($\gt 95 {{\ \rm per\ cent}}$) of galaxies with X-ray luminous AGNs at z = 0.5−3 do not show quenched SF: this suggests that if AGN feedback quenches SF, the associated quenching process takes a significant time to act and the quenched phase sets in after the highly luminous phases of AGN activity.

scholarly journals Size, shade, or shape? The contribution of galaxies of different types to the star formation history of the Universe from SDSS-IV MaNGA

2021 ◽  
Vol 502 (3) ◽  
pp. 3128-3143
Author(s):  
Thomas Peterken ◽  
Alfonso Aragón-Salamanca ◽  
Michael Merrifield ◽  
Vladimir Avila-Reese ◽  
Nicholas F Boardman ◽  
...  
Keyword(s):  
Star Formation ◽  
Sloan Digital Sky Survey ◽  
Star Formation History ◽  
Fourth Generation ◽  
Massive Galaxies ◽  
Formation History ◽  
Galaxy Sample ◽  
History Of ◽  
Stellar Masses ◽  
The Universe

ABSTRACT By fitting stellar populations to the fourth generation of the Sloan Digital Sky Survey (SDSS-IV) Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey observations of ∼7000 suitably weighted individual galaxies, we reconstruct the star formation history of the Universe, which we find to be in reasonable agreement with previous studies. Dividing the galaxies by their present-day stellar mass, we demonstrate the downsizing phenomenon, whereby the more massive galaxies hosted the most star formation at earlier times. Further dividing the galaxy sample by colour and morphology, we find that a galaxy’s present-day colour tells us more about its historical contribution to the cosmic star formation history than its current morphology. We show that downsizing effects are greatest among galaxies currently in the blue cloud, but that the level of downsizing in galaxies of different morphologies depends quite sensitively on the morphological classification used, due largely to the difficulty in classifying the smaller low-mass galaxies from their ground-based images. Nevertheless, we find agreement that among galaxies with stellar masses $M_{\star } \gt 6\times 10^{9}\, \mathrm{ M}_{\odot }$, downsizing is most significant in spirals. However, there are complicating factors. For example, for more massive galaxies, we find that colour and morphology are predictors of the past star formation over a longer time-scale than in less massive systems. Presumably this effect is reflecting the longer period of evolution required to alter these larger galaxies’ physical properties, but shows that conclusions based on any single property do not tell the full story.

scholarly journals LARgE Survey – II. The dark matter haloes and the progenitors and descendants of ultramassive passive galaxies at cosmic noon

2020 ◽  
Vol 494 (1) ◽  
pp. 804-818 ◽  
Author(s):  
Gurpreet Kaur Cheema ◽  
Marcin Sawicki ◽  
Liz Arcila-Osejo ◽  
Anneya Golob ◽  
Thibaud Moutard ◽  
...  
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Galaxy Clusters ◽  
High Redshift ◽  
Massive Galaxies ◽  
Galaxy Population ◽  
Stellar Masses ◽  
Large Survey ◽  
Massive Galaxy ◽  
Comparable Mass

ABSTRACT We use a 27.6 deg2 survey to measure the clustering of gzKs-selected quiescent galaxies at z ∼ 1.6, focusing on ultramassive quiescent galaxies. We find that z ∼ 1.6 Ultra-Massive Passively Evolving Galaxies (UMPEGs), which have Ks(AB) &lt; 19.75 (stellar masses of M⋆$\gtrsim10^{11.4}\,\mathrm{ M}_{\odot }$ and mean &lt;M⋆&gt;  = 1011.5 M⊙), cluster more strongly than any other known galaxy population at high redshift. Comparing their correlation length, r0 = 29.77 ± 2.75h−1Mpc, with the clustering of dark matter (DM) haloes in the Millennium XXL N-body simulation suggests that these z ∼ 1.6 UMPEGs reside in DM haloes of mass Mh ∼ 1014.1h−1M⊙. Such very massive z ∼ 1.6 haloes are associated with the ancestors of z ∼ 0 massive galaxy clusters such as the Virgo and Coma clusters. Given their extreme stellar masses and lack of companions with comparable mass, we surmise that these UMPEGs could be the already-quenched central massive galaxies of their (proto)clusters. We conclude that with only a modest amount of further growth in their stellar mass, z ∼ 1.6 UMPEGs could be the progenitors of some of the massive central galaxies of present-day massive galaxy clusters observed to be already very massive and quiescent near the peak epoch of the cosmic star formation.

scholarly journals The VIMOS VLT Deep Survey: A census of active and passive galaxies to redshift 1.3

2006 ◽  
Vol 2 (S235) ◽  
pp. 400-400
Author(s):  
D. Vergani
Keyword(s):  
Star Formation ◽  
Cosmic Time ◽  
Late Type ◽  
Limited Sample ◽  
Active Star ◽  
Star Forming ◽  
Star Formation Activity ◽  
Deep Survey ◽  
Stellar Masses ◽  
The Universe

AbstractWe are studying how stellar masses assemble through cosmic time since the Universe had only 30% of its present age. We are conducting a census of galaxies which covers the end of the most active star-forming phase, using a mass-limited sample of approximately 5,000 objects selected from the VIMOS VLT Deep Survey (VVDS) in the redshift range 0.45 < z < 1.3. With a criterion based on the direct spectral measurement of the 4000Å Balmer break, Dn(4000), we have classified our sample in spectroscopically early and late-type galaxies. The trends existing between stellar mass, spectroscopic classification, and star formation activity are clearly shown in our analysis.

scholarly journals Correlations between H α equivalent width and galaxy properties at z = 0.47: Physical or selection-driven?

2021 ◽  
Vol 503 (4) ◽  
pp. 5115-5133
Author(s):  
A A Khostovan ◽  
S Malhotra ◽  
J E Rhoads ◽  
S Harish ◽  
C Jiang ◽  
...  
Keyword(s):  
Star Formation ◽  
Equivalent Width ◽  
Luminosity Function ◽  
Mass Function ◽  
Stellar Mass ◽  
High Mass ◽  
Selection Effects ◽  
Star Formation Activity ◽  
Low Mass ◽  
Stellar Masses

ABSTRACT The H α equivalent width (EW) is an observational proxy for specific star formation rate (sSFR) and a tracer of episodic, bursty star-formation activity. Previous assessments show that the H α EW strongly anticorrelates with stellar mass as M−0.25 similar to the sSFR – stellar mass relation. However, such a correlation could be driven or even formed by selection effects. In this study, we investigate how H α EW distributions correlate with physical properties of galaxies and how selection biases could alter such correlations using a z = 0.47 narrow-band-selected sample of 1572 H α emitters from the Ly α Galaxies in the Epoch of Reionization (LAGER) survey as our observational case study. The sample covers a 3 deg2 area of COSMOS with a survey comoving volume of 1.1 × 105 Mpc3. We assume an intrinsic EW distribution to form mock samples of H α emitters and propagate the selection criteria to match observations, giving us control on how selection biases can affect the underlying results. We find that H α EW intrinsically correlates with stellar mass as W0∝M−0.16 ± 0.03 and decreases by a factor of ∼3 from 107 M⊙ to 1010 M⊙, while not correcting for selection effects steepens the correlation as M−0.25 ± 0.04. We find low-mass H α emitters to be ∼320 times more likely to have rest-frame EW&gt;200 Å compared to high-mass H α emitters. Combining the intrinsic W0–stellar mass correlation with an observed stellar mass function correctly reproduces the observed H α luminosity function, while not correcting for selection effects underestimates the number of bright emitters. This suggests that the W0–stellar mass correlation when corrected for selection effects is physically significant and reproduces three statistical distributions of galaxy populations (line luminosity function, stellar mass function, EW distribution). At lower stellar masses, we find there are more high-EW outliers compared to high stellar masses, even after we take into account selection effects. Our results suggest that high sSFR outliers indicative of bursty star formation activity are intrinsically more prevalent in low-mass H α emitters and not a byproduct of selection effects.

Sign in / Sign up

Export Citation Format

Share Document