THE BARYON CONTENT OF COSMIC STRUCTURES

By S. McGaugh, J. Schombert, W. D. de Blok, Matthew J. Zagursky. 2009

194 citations recorded by the source corpus.

We make an inventory of the baryonic and gravitating mass in structures ranging from the smallest galaxies to rich clusters of galaxies. We find that the fraction of baryons converted to stars reaches a maximum between M500 = 1012 and 1013 M☉, suggesting that star formation is most efficient in bright galaxies in groups. The fraction of baryons detected in all forms deviates monotonically from the cosmic baryon fraction as a function of mass. On the largest scales of clusters, most of the expected baryons are detected, while in the smallest dwarf galaxies, fewer than 1% are detected. Where these missing baryons reside is unclear.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b16bc1cceb5d7c881dbb1db0c44f62253f2df500

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Citations in the corpus

Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “In particular, what fraction of baryons are condensed into stars as opposed to spreading out in the form of gas and dust in and outside of galaxies (Cen & Ostriker 1999; McGaugh et al. 2010; Putman et al. 2012; Shull et al. 2012)?”
Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, background): “Even when adding together the mass of all stars to the mass of the ISM, observed galaxies generally do not appear to contain their share of available baryons in the cosmological context (Fukugita, Hogan & Peebles 1998; McGaugh et al. 2010).”
Cosmic ray driven outflows in global galaxy disc models (2013, unknown): “These estimates also agree reasonably well with the dark matter content of individual galaxies estimated either with rotation curves (e.g. McGaugh et al. 2000, 2010; Stark, McGaugh & Swaters 2009) or weak lensing (e.g. Mandelbaum E-mail: msalem@astro.columbia.edu (MS); gbryan@astro.columbia.edu…”
Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, background): “Measurements are referenced to the radius R500 where the enclosed density is 500 times the cosmic mean [284].”
The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, unknown): “Previous studies (Zaritsky et al. 2006, 2008; McGaugh et al. 2010; Dutton et al. 2011a) have tried to unify dynamical scaling relations of spiral galaxies and ETGs.”
The neutral hydrogen content of galaxies in cosmological hydrodynamic simulations (2013, background): “The former discrepancy arises because there are no outflows to eject material from lowmass galaxies, and hence the baryon fraction in these systems is very large (Davé 2009), in disagreement with observations that show a small baryon content in dwarfs (e.g. McGaugh et al. 2010).”
Mass models of the Milky Way (2011, background): “McGaugh et al. (2010) found log10 Mbaryon = 4.0 log10 Vc + 1.65 for disc galaxies, with a scatter that is entirely consistent with observational uncertainty, where 1.1 × Vc was the actual observed circular speed.”
THE BARYONIC TULLY–FISHER RELATION OF GAS-RICH GALAXIES AS A TEST OF ΛCDM AND MOND (2011, result): “This value is of course very similar to the unweighted value (45 M⊙ km −4 s4) obtained from the Stark et al. (2009) sample alone (McGaugh et al. 2010; McGaugh & Wolf 2010).”
The Circumgalactic Medium (2017, background): “Even at their most “efficient”, L ∗ galaxies have converted only ∼ 20% of their halos’ baryons into stars (Figure 2c), with values of only about 5-10% in sub-L∗ and super-L∗ galaxies (Behroozi, Conroy & Wechsler 2010; McGaugh et al. 2010).”
THE COS-HALOS SURVEY: PHYSICAL CONDITIONS AND BARYONIC MASS IN THE LOW-REDSHIFT CIRCUMGALACTIC MEDIUM (2014, background): “The gas in the ISM of these galaxies will vary from very little to nearly as much as the stellar contribution (McGaugh et al. 2010; Martin et al. 2010).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, methodology): “The BTF relation has been investigated over the years (McGaugh et al. 2000, 2010; Bell & de Jong 2001; Verheijen 2001; McGaugh 2005; Stark et al. 2009).”
How supernova feedback turns dark matter cusps into cores (2011, background): “The winds have been shown to be important in matching the star formation rates, distribution of stars and final baryon fractions of the dwarf galaxies (see McGaugh et al. 2010; Brook et al. 2011; Oh et al. 2011a).”
The formation of disc galaxies in a ΛCDM universe (2010, background): “Similar to the photometric TF is the ‘baryonic TF’ relation (McGaugh et al. 2000, 2010) which links characteristic rotation velocity with total galaxy baryonic mass.”
AN EMPIRICAL CHARACTERIZATION OF EXTENDED COOL GAS AROUND GALAXIES USING Mg ii ABSORPTION FEATURES (2010, background): “Furthermore, the cool clouds together with the confining hot medium offer a reservoir for missing baryons in individual galactic halos (e.g. McGaugh et al. 2010).”
DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, background): “The winds clearly affect the chemical evolution of galaxies, but their role (if any) in creating the observed baryon deficit remains unclear (e.g., McGaugh et al. 2010).”
Gaseous Galaxy Halos (2012, background): “…is substantially smaller than the cosmic mean (∼ 0.4 for the Milky Way), and this is attributed to powerful outflow mechanisms (Bregman, 2007; McGaugh et al., 2010), as is the ability to reproduce the basic properties of a galaxy in cosmological simulations (Benson et al., 2003; McCarthy et…”
Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, background): “But these scenarios must explain IGM enrichment separately, and must hide most of the gravitationally-accreted baryons in halos in some undetected form which is becoming increasingly difficult to accomodate (e.g. McGaugh et al. 2010; Dai et al. 2010).”
Quenching and ram pressure stripping of simulated Milky Way satellite galaxies (2017, background): “These systems also pose challenges to models of galaxy formation, as many appear to be some of the most dark matter dominated objects in the Universe (McGaugh et al. 2010).”
The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, background): “…related to Hypothesis 0ii which plagues all known BB-based cosmological models are the two missing baryon problems (e.g. Anderson & Bregman 2010; McGaugh et al. 2010): (i) From BB-nucleosynthesis and CMB observations the cosmic average baryon-to-DMmass-density fraction is fb, DM¼ 0.171 0.006…”