Photoionization Feedback in Low-Mass Galaxies at High Redshift

By M. Dijkstra, Zoltán Haiman, Martin J. Rees, D. Weinberg. 2003

229 citations recorded by the source corpus.

The cosmic ultraviolet ionizing background impacts the formation of dwarf galaxies in the low-redshift universe (z ≲ 3) by suppressing gas infall into galactic halos with circular velocities up to vcirc ~ 75 km s-1. Using a one-dimensional, spherically symmetric hydrodynamics code (Thoul & Weinberg), we examine the effect of an ionizing background on low-mass galaxies forming at high redshifts (z ≳ 10). We find that the importance of photoionization feedback is greatly reduced because (1) at high redshift, dwarf galaxy-sized objects can self-shield against the ionizing background, (2) collisional cooling processes at high redshift are more efficient, (3) the amplitude of the ionizing background at high redshift is lower, and (4) the ionizing radiation turns on when the perturbation that will become the dwarf galaxy has already grown to a substantial overdensity. We find that because of these reasons, gas can collect inside halos with circular velocities as low as vcirc ~ 10 km s-1 at z > 10. This result has important implications for the reionization history of the universe.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/26de30f37d543e36e1ca8b495bbe3cc8358b1f5e

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Citations in the corpus

Fluctuations in the high-redshift Lyman–Werner background: close halo pairs as the origin of supermassive black holes (2008, background): “Ionization and heating by photons with energies exceeding the hydrogen ionization threshold E > EH affect the ability of gas to cool and collapse into dense objects (e.g Couchman & Rees 1986; Efstathiou 1992; Thoul & Weinberg 1996; Kitayama & Ikeuchi 2000; Dijkstra et al. 2004).”
H i IN LOCAL GROUP DWARF GALAXIES AND STRIPPING BY THE GALACTIC HALO (2009, background): “The mass scale for the halos that are able to accrete gas from the IGM after reionization is somewhat uncertain (Dijkstra et al. 2004), however the gas-rich, low mass Leo T is difficult to explain unless its dark matter halo extends out to much larger radii than the observed baryons.”
THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, background): “…be due either to photo-heating associated with the fresh UV background after reionization (e.g. Thoul & Weinberg 1996; Quinn et al. 1996; Barkana & Loeb 1999; Gnedin 2000; Dijkstra et al. 2004), or to SN feedback (e.g. Dekel & Silk 1986; Dutton & van den Bosch 2009; Oppenheimer & Davé 2008) 10.”
Escape of Ionizing Radiation from High-Redshift Galaxies (2007, background): “…2000; Schaye et al. 2000; McDonald et al. 2001; Fechner & Reimers 2007), reducing gas accretion onto small dwarf galaxies (Efstathiou 1992; Thoul & Weinberg 1996; Dijkstra et al. 2004), and evaporating the existing gas in small halos (Barkana & Loeb 1999; Shaviv & Dekel 2003; Shapiro et al. 2004).”
The global 21-centimeter background from high redshifts (2006, background): “Each assumes that the minimum virial temperature increases to Th = 2 × 105 K in ionized regions, near the upper limit of theoretical expectations (Dijkstra et al. 2004b).”
Two populations of metal-free stars in the early Universe (2006, background): “Specifically, Dijkstra et al. (2004) showed that suppression of gas infall is not as efficient in the high-redshift universe as it is for z .”
The first galaxies : assembly, cooling and the onset of turbulence (2008, background): “Related to this, they have the ability to retain gas photoheated by hydrogen ionization (Dijkstra et al. 2004), likely allowing self-regulated star formation for the first time.”
Self-regulated reionization (2006, methodology): “On the other hand, Dijkstra et al. (2004) recently showed, using the same method as Thoul & Weinberg (1996), that at high redshifts the suppression is not as effective, and somewhat smaller galaxies can stillre ain some cooled gas.”
THE ASSEMBLY OF SUPERMASSIVE BLACK HOLES AT HIGH REDSHIFTS (2008, background): “Such halos could continue to form BHs if heating by the UV background is the primary mechanism for seed suppression, as they are able to shield their central gas from the UV radiation (Dijkstra et al. 2004).”
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift (2013, background): “…for much smaller halos, where gas is optically thin to UV radiation, such that radiation pressure has little effect and the gas can be easily photoevaporated by photoheating (Thoul & Weinberg 1996; Quinn et al. 1996; Barkana & Loeb 1999; Gnedin 2000; Dijkstra et al. 2004; Governato et al. 2007).”
Ubiquitous seeding of supermassive black holes by direct collapse (2012, methodology): “In accordance with Dijkstra et al. (2004), a circular velocity threshold ofVc = 20 km s−1 was added on top of the fiducial model to account for the reionisation feedback in haloes withTvir > 104 K between6 < z < 11.”
Efficient Simulations of Early Structure Formation and Reionization (2007, unknown): “2000b, ApJ, 542, 535 Haiman, Z., & Bryan, G. L. 2006, ApJ, 650, 7 Haiman, Z., Rees, M. J., & Loeb, A. 1997, ApJ, 484, 985 Hockney, R. W., & Eastwood, J. W. 1988, Computer simulation using particles (Bristol: Hilger, 1988) Iliev, I. T. et al. 2006a, MNRAS, submitted, preprint astro- ph/0603199 Iliev,”
Dark Matter Subhalos and the Dwarf Satellites of the Milky Way (2008, background): “…has been the subject of many studies, and depends on the redshift of collapse, the amplitude and spectrum of the ionizing background, and the ability of the system to self-shield against UV radiation (e.g. Efstathiou 1992; Thoul & Weinberg 1996; Navarro & Steinmetz 1997; Dijkstra et al. 2004).”
The morphology of H ii regions during reionization (2006, background): “The collapsing gas is already significantly overdense prior to front-crossing, giving it a large collisional cooling rate and possibly allowing it to self-shield (Dijkstra et al. 2004).”
LOWER-LUMINOSITY GALAXIES COULD REIONIZE THE UNIVERSE: VERY STEEP FAINT-END SLOPES TO THE UV LUMINOSITY FUNCTIONS AT z ⩾ 5–8 FROM THE HUDF09 WFC3/IR OBSERVATIONS (2011, methodology): “In deriving the SFR density, we integrate the LF down to −10mag, given the likely supression of galaxy formation at smaller scales from the UV background, SNe feedback, and inefficient gas cooling (e.g., Read et al. 2006; Dijkstra et al. 2004).”
INTENSITY MAPPING WITH CARBON MONOXIDE EMISSION LINES AND THE REDSHIFTED 21 cm LINE (2011, background): “Feedback from photoionization and supernovae explosions may, however, limit the efficiency of star formation in these small mass halos, raising Msf,min, although the precise impact of these effects is still unclear (e.g. Dijkstra et al. 2004).”
REIONIZATION AFTER PLANCK: THE DERIVED GROWTH OF THE COSMIC IONIZING EMISSIVITY NOW MATCHES THE GROWTH OF THE GALAXY UV LUMINOSITY DENSITY (2015, background): “Faintward of −13 mag, galaxy formation may be suppressed due to the inefficient gas cooling onto low-mass halos (e.g., Rees & Ostriker 1977) or due to the difficulties in low-mass galaxies retaining their gas (e.g., Mac Low & Ferrara 1999; Dijkstra et al. 2004).”