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ELVES-Field: Isolated Dwarf Galaxy Quenched Fractions Rise below M∗ ≈ 107 M⊙
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DOI：10.3847/2041-8213/ae4bdf.png)
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Abstract
En 中文
We use a new sample of low-mass (M-* < 10(9) M-circle dot) isolated galaxies from the Exploration of Local VolumE Survey-Field (ELVES-Field) to examine the star formation properties and sizes of field dwarf galaxies in the Local Volume (LV; D < 10 Mpc). This volume-limited sample was selected from nearly 3000 deg(2) of imaging, relying on surface brightness fluctuations to determine distances to the majority of the systems and is complete to M-* approximate to 10(6) M-circle dot. Across the surveyed area, we catalog over 2300 candidate LV dwarfs, of which we confirm 95 as genuine LV members and reject over 1600 as background contaminants, with the remaining 600 candidates still requiring a distance measurement. Of the confirmed LV dwarfs, 46 are either new discoveries or confirmed via a distance measurement for the first time here. We explore different environmental criteria to select isolated dwarfs but primarily focus on dwarfs that are >2 & times; R-vir in projection from any known group with M-star > 10(9)M(circle dot). We find that, at higher dwarf masses (M-star greater than or similar to 10(7)M(circle dot)), essentially all field dwarfs are star forming as has been found before. In contrast, at M-star less than or similar to 10(7)M(circle dot), similar to 30% of field dwarfs appear to be quenched. Finally, we find that isolated dwarfs are noticeably smaller (similar to 20%) than satellite dwarfs of the same stellar mass, regardless of quenched status.
Keywords:
BRIGHTNESS FLUCTUATION DISTANCES
STAR-FORMATION PROPERTIES
GENERATION VIRGO CLUSTER
101 SATELLITE SYSTEMS
HALO MASS RELATION
LOCAL GROUP
LUMINOSITY FUNCTION
RAM PRESSURE
SURVEY. III.
GAS CONTENT
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11.7
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1.2W
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