The first galaxies : assembly, cooling and the onset of turbulence

By Thomas Greif, Jarrett L. Johnson, Ralf Klessen, Volker Bromm. 2008

196 citations recorded by the source corpus.

A B ST R A C T W e investigate the properties oftherst galaxies at z & 10 with highly resolved num ericalsim ulations,starting from cosm ologicalinitialconditions and taking into accountallrelevantprim ordialchem istry and cooling.Arstgalaxy ischaracterized by theonsetofatom ichydrogen cooling,oncethevirialtem peratureexceeds ' 10 4 K, and its ability to retain photoheated gas.W e follow the com plex accretion and star form ation history ofa ' 5 � 10 7 Msystem by m eans ofa detailed m erger tree and derive an upper lim it on the num ber ofPopulation III (Pop III) stars form ed priorto itsassem bly.W e investigate the therm aland chem icalevolution ofinfalling gasandnd thatpartialionization attem peratures & 10 4 K catalysestheform ation ofH2 and hydrogen deuteride,allowing the gas to coolto the tem perature ofthe cosm ic m icrowavebackground.Depending on the strength ofradiative and chem ical feedback,prim ordialstarform ation m ightbedom inated by interm ediate-m assPop III stars form ed during the assem bly oftherst galaxies.Accretion on to the nascent galaxy beginswith hotaccretion,wheregasisaccreted directly from theintergalactic m edium and shock-heated to thevirialtem perature,butisquickly accom panied by a phaseofcold accretion,wherethegascoolsinlam entsbefore owinginto theparent halo with high velocities.Thelatterdrivessupersonicturbulenceatthecentreofthe galaxy and could lead to very ecientchem icalm ixing.The onsetofturbulence in therstgalaxiesthuslikely m arksthetransition to Pop IIstarform ation. K ey w ords: stars:early-type { stars:form ation { galaxies:form ation { galaxies: high-redshift{ cosm ology:theory { early Universe.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/086d70922e9bc30511ed2931d33cc099ee946752

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Formation of supermassive black holes (2010, background): “…hand, ‘external’ conditions determine how much gas is available, at least initially, to the MBH. Cosmological hydrodynamic simulations suggest that gravitational collapse produces dense central gas concentrations in protogalaxies (e.g., Pelupessy et al, 2007; Wise et al, 2008; Greif et al, 2008).”
CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, background): “470 million years old (Wise & Abel 2007; Wise et al. 2008; Greif et al. 2008, 2010; and for recent reviews, see Bromm & Yoshida 2011 and Dunlop 2012).”
Evolution of magnetic fields in galaxies and future observational tests with the Square Kilometre Array (2008, background): “Highly resolved simulations showed that the first galaxies were born at redshifts z 10, after the atomic cooling criterion was fulfilled and they were able to retain the photo-heated gas (Greif et al. 2008).”
Black hole formation in the early Universe (2013, background): “Numerical simulations show that primordial gas becomes turbulent during the formation of the first galaxies (Greif et al. 2008; Wise et al. 2008).”
Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave (2014, background): “Moreover, cosmological simulations studying the hierarchically merging of haloes suggest that most galaxies could include a large number of the mini-haloes where Pop III stars form (e.g. Greif et al. 2008; Bromm & Yoshida 2011; Rashkov et al. 2012).”
Resolving the Formation of Protogalaxies. III. Feedback from the First Stars (2007, methodology): “In structure formation, turbulence can also arise during the virialization of cosmological halos (Wise & Abel 2007; Greif et al. 2008).”
The first stars: formation of binaries and small multiple systems (2009, methodology): “This method was also used in the work of Greif et al. (2008), in which they simulated the formation of a first galaxy beginning from cosmological initial conditions.”
A NEW JEANS RESOLUTION CRITERION FOR (M)HD SIMULATIONS OF SELF-GRAVITATING GAS: APPLICATION TO MAGNETIC FIELD AMPLIFICATION BY GRAVITY-DRIVEN TURBULENCE (2011, background): “…it became clear that primordial gas becomes highly turbulent during the formation of the first galaxies and stars as well (e.g., Abel et al. 2002; O’Shea & Norman 2007; Wise & Abel 2007; Clark et al. 2008; Greif et al. 2008), which has far-reaching consequences for all cosmic structure formation.”
The birth of a galaxy – II. The role of radiation pressure (2012, background): “For example, virial shocks and internal weak shocks have been found to drive turbulence during halo virialization (Wise & Abel 2007a; Greif et al. 2008).”
Small-scale dynamo action during the formation of the first stars and galaxies - I. The ideal MHD limit (2010, methodology): “Radial profiles of the turbulent velocity in the first galaxies indicate that there are some random fluctuations, but the orderof-magnitude of the turbulent velocity does not change during the collapse (Wise & Abel 2007; Greif et al. 2008; Wise et al. 2008).”
Pathways to massive black holes and compact star clusters in pre-galactic dark matter haloes with virial temperatures ≳10 000 K (2008, background): “Especially for the first generation of these haloes it is thus very uncertain, how efficiently they have formed stars (e.g. Greif et al. 2008; Norman 2008; Whalen et al. 2008).”
On the universality of supersonic turbulence (2013, background): “Turbulence in high-redshift galaxies is probably generated during the collapse of primordial haloes and later by the feedback from the first stars (Greif et al. 2008; Green et al. 2010; Latif et al. 2013).”
IONIZING PHOTON ESCAPE FRACTIONS FROM HIGH-REDSHIFT DWARF GALAXIES (2008, background): “The combination of lower temperatures and greater turbulent motions leads to turbulent Mach numbers above unity and close to the circular velocity of the halo, i.e. fturb = 1 (Wise & Abel 2007a; Greif et al. 2008).”
The First Stars (2012, methodology): “One of the most exciting results of the Greif et al. (2011a) model is that some of the protostars that are ejected from the centre of the star-forming minihalo have masses that are below 0.”
Near-Field Cosmology with Extremely Metal-Poor Stars (2015, background): “Detailed numerical simulations of star formation in atomic cooling halos have already suggested where these pathways may occur, although details so far remain unclear (Wise & Abel 2007, Greif et al. 2008, Ritter et al. 2012).”
Ubiquitous seeding of supermassive black holes by direct collapse (2012, background): “The accreting discs of both Pop III remnant BHs and DCBHs could also emit LW photons (e.g. Pelupessy et al. 2007; Alvarez et al. 2009; Jeon et al. 2011), where the emission would depend on both the BH mass and accretion rate (Greif et al. 2008).”
Galaxy formation theory (2010, background): “…et al. 2008; O’Shea and Norman 2007, 2008; Harris et al. 2007; Stacy and Bromm 2007) may be crucialfor understanding how this population of galaxies grows (Tegmark et al. 1997; Ricotti et al. 2001; Wise and Abel 2007a,b; Greif et al. 2008; Wise and Abel 2008b; Wise et al. 2008; Bromm et al. 2009).”