Feedback and the fundamental line of low-luminosity low-surface-brightness/dwarf galaxies

By A. Dekel, J. M. H. U. Jerusalem, U. Columbia. 2002

205 citations recorded by the source corpus.

We study in simple terms the role of feedback in establishing the scaling relations of low-surface-brightness (LSB) and dwarf galaxies with stellar masses in the range 6 × 10 5 ≤ M * ≤ 3 x 10 1 0 M O . . These galaxies - as measured, for example, from the Sloan Digital Sky Survey (SDSS) and in the Local Group - show tight correlations of internal velocity, metallicity and surface brightness (or radius) with M * . They define a fundamental line which distinguishes them from the brighter galaxies of high surface brightness and metallicity. The idealized model assumes spherical collapse of cold dark matter (CDM) haloes to virial equilibrium and angular momentum conservation. The relations for bright galaxies are reproduced by assuming that M * is a constant fraction of the halo mass M. The upper bound to the low-luminosity LSBs coincides with the virial velocity of haloes in which supernova feedback could significantly suppress star formation, V 30 km s - 1 , retain gas-rich discs with feedback-regulated star formation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/345d945b1d4afc2f06d1974bc418e93aff68933e

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. A. Dekel
4. R. Dav'e
5. R. Somerville
6. Volker Springel
7. T. Naab
8. E. Quataert

In Instrumentation

1. P. Hopkins
2. A. Dekel
3. L. Hernquist
4. R. Dav'e
5. R. Somerville
6. T. Naab
7. Thomas J. Cox
8. Volker Springel

Citations in the corpus

• Forming disc galaxies in ΛCDM simulations (2006, background): “…the ultraviolet (UV) background, being able to reduce gas retention and accretion in haloes with low virial temperature, may also solve the problem of the overabundance of satellites (Quinn et al. 1996; Gnedin 2000; Benson et al. 2002; Dekel & Woo 2003; Kravtsov, Gnedin & Klypin 2004; Monaco 2004).”
• Scaling relations and the fundamental line of the local group dwarf galaxies (2008, methodology): “Note also that c© 2006 RAS, MNRAS 000, 1–18 the smallest dwarfs cluster just above V ∼ 10km s−1 and could even be described by a constant V (dash-dotted line) which Dekel & Woo (2003) explain might be due to radiative feedback.”
• Structural Parameters of Thin and Thick Disks in Edge-on Disk Galaxies (2005, background): “…that the lower metallicities and effective yields seen in low-mass galaxies is due to the onset of SN-driven winds at the mass scale at which the metallicity begins to fall (Vc 120 km s 1 or Mbaryon < 3 ;1010 M ; e.g., Garnett 2002; Tremonti et al. 2004; Dekel & Woo 2003; Kauffmann et al. 2003).”
• Tracing Galaxy Formation with Stellar Halos. I. Methods (2005, background): “…of ∼ 104K (corresponding to Vmax ∼ 16kms−1) prevents any gas that could remain bound to these halos from cooling and forming stars (Kepner et al. 1997; Dekel & Woo 2003); finally, even if we were to allow star formation in these 6 systems, their contribution to the stellar halo mass would be…”
• A CATALOG OF GLOBULAR CLUSTER SYSTEMS: WHAT DETERMINES THE SIZE OF A GALAXY'S GLOBULAR CLUSTER POPULATION? (2013, background): “For the most massive galaxies, AGN feedback and virial shock heating of infalling gas will lower the SFE (Dekel & Silk 1986; Dekel & Woo 2003; Dekel & Birnboim 2006; Bower et al. 2006).”
• Mass loss from dwarf spheroidal galaxies: the origins of shallow dark matter cores and exponential surface brightness profiles (2004, background): “…including ram pressure stripping (Einasto et al. 1974; Grebel et al. 2003), supernovae explosions (Larson 1974; Dekel & Silk 1986; Efstathiou 2000; Dekel & Woo 2003); photoevaporation (Quinn, Katz & Efstathiou 1996; Barkana & Loeb 1999); and the effects of galaxy harassment and tidal stripping…”
• Λ Cold Dark Matter, Stellar Feedback, and the Galactic Halo Abundance Pattern (2005, background): “Dekel & Woo (2003) (DW) have used a compilation of dwarf galaxy data to show that the stellar masses and metallicities of dwarf galaxies follow a fairly tight relation,Z ∝ M2/5⋆ , and have argued that blow-out feedback can naturally explain this trend.”
• The Detailed Star Formation History in the Spheroid, Outer Disk, and Tidal Stream of the Andromeda Galaxy (2006, background): “The relatively high metallicity of the stream implies its progenitor was at least as massive as 109 M⊙ (see Dekel & Woo 2003); as such, most numerical simulations of the stream assume it is a dwarf galaxy that was only recently disrupted by close passage to Andromeda, within the last∼0.5 Gyr…”
• Mass, metal, and energy feedback in cosmological simulations (2007, background): “As Dekel & Woo (2003) showed, if the outflow energy couples efficiently to ambient halo gas, this can yield the mass-metallicity relation as observed, as well as other properties of dwarf galaxies.”
• The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, unknown): “14 E.g. listing mostly more recent papers: Dekel & Silk (1986); Dekel & Woo (2003); Tollerud et al. (2008); D’Onghia & Lake (2008); Li & Helmi (2008); Macciò, Kang & Moore (2009); Koposov et al. (2009); Okamoto& Frenk (2009); Kirby et al. (2009); Shaya et al. (2009); Busha et al. (2010); Primack…”
• Constraints on star formation driven galaxy winds from the mass–metallicity relation at z= 0 (2010, result): “Regardless, this need for a high and mass-dependent wind efficiency is in broad agreement with previous studies (Dekel & Woo 2003; Dutton et al. 2010b; Sawala et al. 2010; Spitoni et al. 2010).”
• The Tumultuous Lives of Galactic Dwarfs and the Missing Satellites Problem (2004, background): “10 10 M⊙, similar to the observed range of stellar masses of the LG galaxies (e.g., Dekel & Woo 2003).”
• From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z ~ 2 from Integral Field Spectroscopy in the SINS Survey (2008, methodology): “Following Dekel & Silk (1986) and Dekel & Woo (2003), this critical baryonic mass is given by Mb;crit ¼ 2:0 ; 1010 vd;crit 100 km s 1 3 1þ z 3:2 2”
• A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “In more massive halos where gas is retained and star formation can begin, further suppression is expected from supernova feedback (Dekel & Silk 1986; Benson et al. 2002; Dekel & Woo 2003; Governato et al. 2007).”
• A Revised Model for the Formation of Disk Galaxies: Low Spin and Dark Halo Expansion (2006, background): “This requires α m = 0.18, so that the galaxy mass fraction, m gal , increases with increasing halo mass, as expected, for example, for simple supernova feedback models (e.g., Dekel & Silk 1986; van den Bosch 2002; Dekel & Woo 2003).”
• Gravitational quenching in massive galaxies and clusters by clumpy accretion (2007, background): “…stability threshold of mBE ∼ 108M⊙, where stars can form, is likely to be removed by supernova feedback after the first starburst (Dekel & Silk 1986; Dekel & Woo 2003), and thus be added to the reservoir of gas available for condensing into smaller, stable gas clumps that are more effective in…”
• Galaxy Evolution in Cosmological Simulations with Outflows II: Metallicities and Gas Fractions (2011, background): “…a competition between the galaxy potential well and the outflow velocity to modulate the metals retained within a galaxy (e.g. Dekel & Silk 1986; Dekel & Woo 2003; Tremonti et al. 2004); here, there is no mention of the potential well depth except indirectly via its effects on the mass loading…”