Star Formation and Quenching of Central Galaxies from Stacked Hi Measurements
Hong Guo, Michael G. Jones, Jing Wang, Lin Lin
Abstract
Abstract We quantitatively investigate the dependence of central galaxy H i mass ( M H i ) on the stellar mass ( M * ), halo mass ( M h ), star formation rate (SFR), and central stellar surface density within 1 kpc (Σ 1 ), taking advantage of the H i spectra stacking technique using both the Arecibo Fast Legacy ALFA Survey and the Sloan Digital Sky Survey. We find that the shapes of M H i – M h and M H i – M * relations are remarkably similar for both star-forming and quenched galaxies, with massive quenched galaxies having constantly lower H i masses of around 0.6 dex. This similarity strongly suggests that neither halo mass nor stellar mass is the direct cause of quenching, but rather the depletion of the H i reservoir. While the H i reservoir for low-mass galaxies of M * < 10 10.5 M ☉ strongly increases with M h , more massive galaxies show no significant dependence of M H i with M h , indicating that the main effect of halo is to determine the smooth cold gas accretion. We find that the star formation and quenching of central galaxies are directly regulated by the available H i reservoir, with an average relation of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>SFR</mml:mi> <mml:mo>∝</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> <mml:mspace width="0.10em"/> <mml:mi mathsize="small" mathvariant="normal">I</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2.75</mml:mn> </mml:mrow> </mml:msubsup> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msubsup> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>0.40</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , implying a quasi-steady state of star formation. We further confirm that galaxies are depleted of their H i reservoir once they drop off the star formation main sequence and there is a very tight and consistent correlation between M H i and Σ 1 in this phase, with <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> <mml:mspace width="0.10em"/> <mml:mi mathsize="small" mathvariant="normal">I</mml:mi> </mml:mrow> </mml:msub> <mml:mo>∝</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi mathvariant="normal">Σ</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> . This result is consistent with the compaction-triggered quenching scenario, with galaxies going through three evolutionary phases of cold gas accretion, compaction and post-compaction, and quenching.