A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION

By E. Papastergis, A. Cattaneo, Shan Huang, R. Giovanelli, M. Haynes. 2012

135 citations recorded by the source corpus.

We use both an H i-selected and an optically selected galaxy sample to directly measure the abundance of galaxies as a function of their “baryonic” mass (stars + atomic gas). Stellar masses are calculated based on optical data from the Sloan Digital Sky Survey and atomic gas masses are calculated using atomic hydrogen (H i) emission line data from the Arecibo Legacy Fast ALFA survey. By using the technique of abundance matching, we combine the measured baryonic function of galaxies with the dark matter halo mass function in a ΛCDM universe, in order to determine the galactic baryon fraction as a function of host halo mass. We find that the baryon fraction of low-mass halos is much smaller than the cosmic value, even when atomic gas is taken into account. We find that the galactic baryon deficit increases monotonically with decreasing halo mass, in contrast with previous studies which suggested an approximately constant baryon fraction at the low-mass end. We argue that the observed baryon fractions of low-mass halos cannot be explained by reionization heating alone, and that additional feedback mechanisms (e.g., supernova blowout) must be invoked. However, the outflow rates needed to reproduce our result are not easily accommodated in the standard picture of galaxy formation in a ΛCDM universe.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/93e651ca725191a2f79dc8c65142051d81ec9a0b

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Citations in the corpus

Is there a "too big to fail" problem in the field? (2014, background): “However, the rescaledVh values are fairly realistic for dwarf galaxies, which are typically DM-dominated (e.g. Papastergis et al. 2012; Sawala et al. 2013).”
Galaxy Masses: A Review (2013, methodology): “…stellar mass functions: Bundy et al. 2006; Pozzetti et al. 2010; Maraston et al. 2012) (e.g. dynamical mass functions: Trujillo-Gomez et al. 2011; Papastergis et al. 2011, 2012), constraints on halo masses by statistical techniques such as those involving satellite kinematics (More et al.…”
THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS–METALLICITY RELATION (2014, background): “From measurements of the stellar and gas content of galaxies in the local Universe, we have that Mg ∝∼ √ M∗ (Papastergis et al. 2012; Peeples et al. 2013).”
THE COS-HALOS SURVEY: PHYSICAL CONDITIONS AND BARYONIC MASS IN THE LOW-REDSHIFT CIRCUMGALACTIC MEDIUM (2014, background): “Traditionally, baryon counting in this regime has focused on a galaxy’s stars, cold ISM, and its hot X-ray halo gas (Bell et al. 2003; Klypin et al. 2011; Baldry et al. 2008; Yang et al. 2009; McGaugh et al. 2010; Anderson & Bregman 2010; Papastergis et al. 2012; Gupta et al. 2012).”
Gravitational probes of dark matter physics (2017, background): “from the extrapolated SMHM relation [341, 347, 343, 348, 349].”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, background): “(9) Using a similar approach, Papastergis et al. (2012) find logFg = log(1.366MHI/M⋆) = −0.43 logM⋆ + 3.89, (10) by fitting a power law to data compiled from opticallyselected galaxy samples (Swaters & Balcells 2002; Garnett 2002; Noordermeer et al. 2005; Zhang et al. 2009).”
Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos (2014, methodology): “We approximate the SMF measured by Papastergis et al. (2012) and Baldry et al. (2012) using double Schechter form given by eq.”
THE SIZE–VIRIAL RADIUS RELATION OF GALAXIES (2012, methodology): “109 M originating from the steepening of the stellar mass function at these masses (Baldry et al. 2008, 2012; Papastergis et al. 2012).”
Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties (2017, background): “…stellar mass and (sub)halo mass (Kravtsov et al. 2004; Vale & Ostriker 2004; Conroy, Wechsler & Kravtsov 2006; Shankar et al. 2006; Behroozi, Conroy & Wechsler 2010; Moster et al. 2010; Guo et al. 2010; Rodŕıguez-Puebla, Drory & Avila-Reese 2012; Papastergis et al. 2012; Hearin et al. 2013b).”
(Almost) Dark Galaxies in the ALFALFA Survey: Isolated H i-bearing Ultra-diffuse Galaxies (2017, background): “We note that abundance matching (using the data from Papastergis et al. 2012) implies that galaxies with the baryonic masses of these sources should live in halos with log Mhalo/M &11.1.”