Mass loss of galaxies due to an ultraviolet background

By T. Okamoto, Liang Gao, Tom Theuns. 2008

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We perform cosmological hydrodynamic simulations to determine to what extent galaxies lose their gas due to photoheating from an ionizing background. We find that the characteristic mass at which haloes on average have lost half of their baryons is M c ∼ 6.5 x 10 9 h -1 M ⊙ at z = 0, which corresponds to a circular velocity of 25 km s -1 . This is significantly lower than the filtering mass obtained by the linear theory, which is often used in semi-analytical models of galaxy formation. We demonstrate it is the gas temperature at the virial radius which determines whether a halo can accrete gas. A simple model that follows the merger history of the dark matter progenitors, and where gas accretion is not allowed when this temperature is higher than the virial temperature of the halo, reproduces the results from the simulation remarkably well. This model can be applied to any reionization history, and is easy to incorporate in semi-analytical models.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e587ecad5b0b07481e7ed2a3d8c249172d052f37

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Citations in the corpus

A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, methodology): “Okamoto et al. (2008) use hydrodynamical simulations to identify the characteristic halo mass, Mchar, that retains 50% of the cosmic baryon fraction, fbar, as a function of z.”
A QUANTITATIVE EXPLANATION OF THE OBSERVED POPULATION OF MILKY WAY SATELLITE GALAXIES (2009, background): “The lower values of Vcrit are favored by the numerical studies of Hoeft et al. (2006) and Okamoto et al. (2008).”
The current status of galaxy formation (2012, background): “Hydrodynamical simulations indicate that this lower limit is sharp (Gnedin, 2000; Okamoto et al., 2008).”
WHAT NEXT-GENERATION 21 cm POWER SPECTRUM MEASUREMENTS CAN TEACH US ABOUT THE EPOCH OF REIONIZATION (2013, background): “…as to which halos host significant stellar populations (see e.g. Haiman et al. 1996, Abel et al. 2002 and Bromm et al. 2002 for lower mass limits on star-forming halos, and e.g. Mesinger & Dijkstra 2008 and Okamoto et al. 2008 for feedback effects which can suppress low mass halo star formation).”
PRE-REIONIZATION FOSSILS, ULTRA-FAINT DWARFS, AND THE MISSING GALACTIC SATELLITE PROBLEM (2008, background): “This value of the circular velocity is also very close to estimates based on the suppression of star formation in dwarfs after reionization (Gnedin 2000; Okamoto et al. 2008).”
Galaxy formation theory (2010, background): “…approach (Thacker and Couchman 2000; Kay et al. 2002; Marri and White 2003; White 2004; Stinson et al. 2006; Cox et al. 2006; Scannapieco et al. 2006a; Tasker and Bryan 2006; Stinson 2007; Vecchia and Schaye 2008; Oppenheimer and Davé 2008; Okamoto et al. 2008b; Booth and Schaye 2009; Ciotti 2009).”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, methodology): “Here we use a table of MF (z) kindly provided by Okamoto et al. (2008) from their simulations; MF varies from ∼ 6.5 × 109M⊙ at z = 0 to ∼ 10 7M⊙ just after reionization at z ∼ 8.”
Is there a "too big to fail" problem in the field? (2014, background): “…et al. 2010; Trujillo-Gomez et al. 2013) and environmental mechanisms (such as photoionization feedback, tidal and ram-pressure stripping, etc.;e.g Okamoto et al. 2008; Arraki et al. 2014; Zolotov et al. 2012; Collins et al. 2013; Kravtsov et al. 2004) that are expected to inhibit the formation…”
The Milky Way’s bright satellites as an apparent failure of ΛCDM (2011, background): “For comparison, we also show Tvir(z) = 10 4 K (the temperature at which primordial gas can cool via atomic transitions) and 105 K (dashed lines), as well as the mass Mc(z) below which at least half of a halo’s baryons have been removed by photo-heating from the UV background (Okamoto et al. 2008).”
Inferring the astrophysics of reionization and cosmic dawn from galaxy luminosity functions and the 21-cm signal (2018, background): “…galaxies is expected to be quenched due to SNe feedback, photo-heating feedback, or inefficient gas accretion (e.g Shapiro et al. 1994; Giroux et al. 1994; Hui & Gnedin 1997; Barkana & Loeb 2001; Springel & Hernquist 2003; Okamoto et al. 2008; Mesinger & Dijkstra 2008; Sobacchi & Mesinger 2013a,b).”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, result): “17 we compare our result for the baryon fraction of halos to the predictions at z = 0 of a cosmological hydrodynamic simulation that includes heating from a photoionizing UV background (Okamoto et al. 2008, black dotted-dashed curve).”
Signatures of X-rays in the early Universe (2012, background): “…and/or mechanical feedback (e.g. Springel & Hernquist 2003) eventually suppresses star formation inside Tvir ∼< 10 5 K halos, though the details and timing of these processes are not well understood at high redshifts (e.g. Mesinger & Dijkstra 2008; Okamoto et al. 2008; Pawlik & Schaye 2009)8.”
THE CENTRAL SLOPE OF DARK MATTER CORES IN DWARF GALAXIES: SIMULATIONS VERSUS THINGS (2010, background): “At even smaller halo masses (Vc < 20-40 km s −1) the collapse of baryons is largely suppressed by the cosmic UV field (Quinn et al. 1996; Okamoto et al. 2008; Gnedin 2010).”