scholarly journals Multi-wavelength mock galaxy catalogs of the low-redshift Universe

2021 ◽  
Author(s):  
Aseem Paranjape ◽  
Tirthankar Roy Choudhury ◽  
Ravi K Sheth
Keyword(s):  
Luminosity Function ◽  
Cross Correlation ◽  
Neutral Hydrogen ◽  
Mass Function ◽  
Stellar Mass ◽  
Scaling Relation ◽  
Radial Acceleration ◽  
Multi Wavelength ◽  
Galaxy Assembly ◽  
Halo Occupation Distribution

Abstract We present a new suite of mock galaxy catalogs mimicking the low-redshift Universe, based on an updated halo occupation distribution (HOD) model and a scaling relation between optical properties and the neutral hydrogen (Hi) content of galaxies. Our algorithm is constrained by observations of the luminosity function and luminosity- and colour-dependent clustering of SDSS galaxies, as well as the Hi mass function and Hi-dependent clustering of massive Hi-selected galaxies in the ALFALFA survey. Mock central and satellite galaxies with realistic values of r-band luminosity, g − r and u − r colour, stellar mass and Hi mass are populated in an N-body simulation, inheriting a number of properties of the density and tidal environment of their host halos. The host halo of each central galaxy is also ‘baryonified’ with realistic spatial distributions of stars as well as hot and cold gas, along with the corresponding rotation curve. Our default HOD assumes that galaxy properties are a function of group halo mass alone, and can optionally include effects such as galactic conformity and colour-dependent galaxy assembly bias. The mocks predict the relation between the stellar mass and Hi mass of massive Hi galaxies, as well as the 2-point cross-correlation function of spatially co-located optical and Hi-selected samples. They enable novel null tests for galaxy assembly bias, provide predictions for the Hi velocity width function, and clarify the origin and universality of the radial acceleration relation in the ΛCDM framework.

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>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.

scholarly journals Evolution of the Stellar Mass Function and Infrared Luminosity Function of Galaxies since z = 1.2

2019 ◽  
Vol 873 (1) ◽  
pp. 78 ◽  
Author(s):  
Richard Beare ◽  
Michael J. I. Brown ◽  
Kevin Pimbblet ◽  
Edward N. Taylor
Keyword(s):  
Luminosity Function ◽  
Mass Function ◽  
Stellar Mass

scholarly journals Clues to the nature of dark matter from first galaxies

2019 ◽  
Vol 489 (1) ◽  
pp. 487-496 ◽  
Author(s):  
Boyan K Stoychev ◽  
Keri L Dixon ◽  
Andrea V Macciò ◽  
Marvin Blank ◽  
Aaron A Dutton
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Galaxy Formation ◽  
Cold Dark Matter ◽  
High Redshift ◽  
Formation Rate ◽  
Neutral Hydrogen ◽  
Mass Function ◽  
Stellar Mass ◽  
The Impact

ABSTRACT We use 38 high-resolution simulations of galaxy formation between redshift 10 and 5 to study the impact of a 3 keV warm dark matter (WDM) candidate on the high-redshift Universe. We focus our attention on the stellar mass function and the global star formation rate and consider the consequences for reionization, namely the neutral hydrogen fraction evolution and the electron scattering optical depth. We find that three different effects contribute to differentiate warm and cold dark matter (CDM) predictions: WDM suppresses the number of haloes with mass less than few 109 M⊙; at a fixed halo mass, WDM produces fewer stars than CDM, and finally at halo masses below 109 M⊙, WDM has a larger fraction of dark haloes than CDM post-reionization. These three effects combine to produce a lower stellar mass function in WDM for galaxies with stellar masses at and below 107 M⊙. For z > 7, the global star formation density is lower by a factor of two in the WDM scenario, and for a fixed escape fraction, the fraction of neutral hydrogen is higher by 0.3 at z ∼ 6. This latter quantity can be partially reconciled with CDM and observations only by increasing the escape fraction from 23 per cent to 34 per cent. Overall, our study shows that galaxy formation simulations at high redshift are a key tool to differentiate between dark matter candidates given a model for baryonic physics.

scholarly journals ACCESS: NIR luminosity function and stellar mass function of galaxies in the Shapley supercluster environment

2010 ◽  
Vol 402 (2) ◽  
pp. 753-766 ◽  
Author(s):  
P. Merluzzi ◽  
A. Mercurio ◽  
C. P. Haines ◽  
R. J. Smith ◽  
G. Busarello ◽  
...  
Keyword(s):  
Luminosity Function ◽  
Mass Function ◽  
Stellar Mass

scholarly journals The Stellar Luminosity Function and Binary Stars

1992 ◽  
Vol 135 ◽  
pp. 234-237
Author(s):  
Pavel Kroupa ◽  
Christopher A. Tout ◽  
Gerard Gilmore
Keyword(s):  
Binary Stars ◽  
Luminosity Function ◽  
Binary Systems ◽  
Small Volume ◽  
Mass Function ◽  
Stellar Mass ◽  
The Sun ◽  
Single Star ◽  
Luminosity Functions ◽  
Low Mass

AbstractIf all stars within a small volume surrounding the sun are counted we obtain an approximation of the low-mass single-star luminosity function. Alternatively, deep photographic surveys cannot resolve most of the binary systems, and consequently we obtain an approximation to the system luminosity function. Comparing the single-star and system luminosity functions we derive the stellar mass function and constrain the properties of binary systems.

scholarly journals An HI Survey of LSB galaxies selected from the APM Survey

1999 ◽  
Vol 171 ◽  
pp. 307-314 ◽  
Author(s):  
Stéphanie Côté ◽  
Tom Broadhurst ◽  
Jon Loveday ◽  
Shannon Kolind
Keyword(s):  
Total Mass ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Neutral Hydrogen ◽  
Mass Function ◽  
Low Surface Brightness ◽  
Redshift Survey ◽  
First Time ◽  
Lsb Galaxies ◽  
Negligible Contribution

AbstractWe present preliminary results of a neutral hydrogen (HI) redshift survey to find Low Surface Brightness (LSB) galaxies in the very nearby universe. Our sample consists of all galaxies in the APM catalog (Maddox et al. 1990) with a mean surface brightness of μ ≥ 24 mag/arcsec2, down to a magnitude limit of bj ≤ 17. With the Parkes 64m radiotelescope 35 objects were detected at v < 4300 km s−1. The resulting luminosity function, HI mass function, and for the first time total mass function are presented. It is found that LSBs make a negligible contribution to the overall integrated luminosity, HI mass, and total mass contained in galaxies.

scholarly journals H i gas content of SDSS galaxies revealed by ALFALFA: implications for the mass–metallicity relation and the environmental dependence of H i in the local Universe

2020 ◽  
Vol 496 (1) ◽  
pp. 111-124 ◽  
Author(s):  
Ying Zu
Keyword(s):  
Star Formation ◽  
Formation Rate ◽  
Neutral Hydrogen ◽  
Mass Function ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Gas Content ◽  
Local Universe ◽  
The Impact ◽  
Environmental Dependence

ABSTRACT The neutral hydrogen (H i) gas is an important barometer of recent star formation and metal enrichment activities in galaxies. I develop a novel statistical method for predicting the H i-to-stellar mass ratio, $f_{\mathrm{H\,{\small I}}}$, of galaxies from their stellar mass and optical colour, and apply it to a volume-limited galaxy sample jointly observed by the Sloan Digital Sky Survey and the Arecibo Legacy Fast ALFA survey. I eliminate the impact of the Malmquist bias against H i-deficient systems on the $f_{\mathrm{H\,{\small I}}}$ predictor by properly accounting for the H i detection probability of each galaxy in the analysis. The best-fitting $f_{\mathrm{H\,{\small I}}}$ predictor, with an estimated scatter of 0.272 dex, provides excellent description to the observed H i mass function. After defining an H i excess parameter as the deviation of the observed $f_{\mathrm{H\,{\small I}}}$ from the expected value, I confirm that there exists a strong secondary dependence of the mass–metallicity relation on H i excess. By further examining the 2D metallicity distribution on the specific star formation rate (sSFR) versus H i excess plane, I show that the metallicity dependence on H i is likely more fundamental than that on sSFR. In addition, I find that the environmental dependence of H i in the local Universe can be effectively described by the cross-correlation coefficient between H i excess and the red galaxy overdensity ρcc = − 0.18. This weak anticorrelation also successfully explains the observed dependence of H i clustering on $f_{\mathrm{H\,{\small I}}}$. My method provides a useful framework for learning H i gas evolution from the synergy between future H i and optical galaxy surveys.

scholarly journals Simulating the effect of photoheating feedback during reionization

2019 ◽  
Vol 488 (1) ◽  
pp. 419-437 ◽  
Author(s):  
Xiaohan Wu ◽  
Rahul Kannan ◽  
Federico Marinacci ◽  
Mark Vogelsberger ◽  
Lars Hernquist
Keyword(s):  
Star Formation ◽  
Galaxy Formation ◽  
Luminosity Function ◽  
High Redshift ◽  
Formation Rate ◽  
Mass Function ◽  
Stellar Mass ◽  
Microwave Background ◽  
Stellar Feedback ◽  
Stellar Sources

Abstract We present self-consistent radiation hydrodynamic simulations of hydrogen reionization performed with arepo-rt complemented by a state-of-the-art galaxy formation model. We examine how photoheating feedback, due to reionization, shapes the galaxies properties. Our fiducial model completes reionization by z ≈ 6 and matches observations of the Ly α forest, the cosmic microwave background electron scattering optical depth, the high-redshift ultraviolet (UV) luminosity function, and stellar mass function. Contrary to previous works, photoheating suppresses star formation rates by more than $50{{\ \rm per\ cent}}$ only in haloes less massive than ∼108.4 M⊙ (∼108.8 M⊙) at z = 6 (z = 5), suggesting inefficient photoheating feedback from photons within galaxies. The use of a uniform UV background that heats up the gas at z ≈ 10.7 generates an earlier onset of suppression of star formation compared to our fiducial model. This discrepancy can be mitigated by adopting a UV background model with a more realistic reionization history. In the absence of stellar feedback, photoheating alone is only able to quench haloes less massive than ∼109 M⊙ at z ≳ 5, implying that photoheating feedback is sub-dominant in regulating star formation. In addition, stellar feedback, implemented as a non-local galactic wind scheme in the simulations, weakens the strength of photoheating feedback by reducing the amount of stellar sources. Most importantly, photoheating does not leave observable imprints in the UV luminosity function, stellar mass function, or the cosmic star formation rate density. The feasibility of using these observables to detect imprints of reionization therefore requires further investigation.

scholarly journals THE GALEX ARECIBO SDSS SURVEY. VII. THE BIVARIATE NEUTRAL HYDROGEN-STELLAR MASS FUNCTION FOR MASSIVE GALAXIES

2013 ◽  
Vol 776 (2) ◽  
pp. 74 ◽  
Author(s):  
Jenna J. Lemonias ◽  
David Schiminovich ◽  
Barbara Catinella ◽  
Timothy M. Heckman ◽  
Sean M. Moran
Keyword(s):  
Neutral Hydrogen ◽  
Mass Function ◽  
Stellar Mass ◽  
Massive Galaxies

scholarly journals A flexible subhalo abundance matching model for galaxy clustering in redshift space

2021 ◽  
Vol 508 (1) ◽  
pp. 175-189
Author(s):  
S Contreras ◽  
R E Angulo ◽  
M Zennaro
Keyword(s):  
Correlation Function ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Stellar Mass ◽  
Tidal Disruption ◽  
Hydrodynamic Simulation ◽  
Hydrodynamical Simulation ◽  
Moderate Resolution ◽  
Galaxy Assembly ◽  
Halo Occupation Distribution

ABSTRACT We develop an extension of subhalo abundance matching (SHAM) capable of accurately reproducing the real and redshift-space clustering of galaxies in a state-of-the-art hydrodynamical simulation. Our method uses a low-resolution gravity-only simulation and it includes orphan and tidal disruption prescriptions for satellite galaxies, and a flexible amount of galaxy assembly bias. Furthermore, it includes recipes for star formation rate (SFR) based on the dark matter accretion rate. We test the accuracy of our model against catalogues of stellar-mass- and SFR-selected galaxies in the TNG300 hydrodynamic simulation. By fitting a small number of free parameters, our extended SHAM reproduces the projected correlation function and redshift-space multipoles for number densities $10^{-3} - 10^{-2}\, h^{3}{\rm Mpc}^{-3}$, at z = 1 and z = 0, and for scales r ∈ [0.3 − 20]h−1Mpc. Simultaneously, the SHAM results also retrieve the correct halo occupation distribution, the level of galaxy assembly bias, and higher order statistics present in the TNG300 galaxy catalogues. As an application, we show that our model simultaneously fits the projected correlation function of the SDSS in three disjoint stellar mass bins, with an accuracy similar to that of TNG300 galaxies. This SHAM extension can be used to get accurate clustering prediction even when using low and moderate-resolution simulations.

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