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Quenching Low-mass Satellite Galaxies: Evidence for a Threshold ICM Density

MPG-Autoren

Roberts,  Ian D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Parker,  Laura C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Brown,  Toby
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Joshi,  Gandhali D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hlavacek-Larrondo,  Julie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wadsley,  James
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Externe Ressourcen

https://ui.adsabs.harvard.edu/abs/2019ApJ...873...42R
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Zitation

Roberts, I. D., Parker, L. C., Brown, T., Joshi, G. D., Hlavacek-Larrondo, J., & Wadsley, J. (2019). Quenching Low-mass Satellite Galaxies: Evidence for a Threshold ICM Density. The Astrophysical Journal, 873.


Zitierlink: https://hdl.handle.net/21.11116/0000-0005-CFEA-B
Zusammenfassung
We compile a sample of Sloan Digital Sky Survey (SDSS) galaxy clusters with high-quality Chandra X-ray data to directly study the influence of the dense intracluster medium (ICM) on the quenching of satellite galaxies. We study the quenched fractions of satellite galaxies as a function of ICM density for low- (109 ≲ M ⋆ ≲ 1010 M ☉), intermediate- (1010 ≲ M ⋆ ≲ 1010.5 M ☉), and high-mass (M ⋆ ≳ 1010.5 M ☉) satellite galaxies with >3000 satellite galaxies across 24 low-redshift (z < 0.1) clusters. For low-mass galaxies we find evidence for a broken power-law trend between satellite quenched fraction and local ICM density. The quenched fraction increases modestly at ICM densities below a threshold before increasing sharply beyond this threshold toward the cluster center. We show that this increase in quenched fraction at high ICM density is well matched by a simple, analytic model of ram pressure stripping. These results are consistent with a picture where low-mass cluster galaxies experience an initial, slow-quenching mode driven by steady gas depletion, followed by rapid quenching associated with ram pressure of cold-gas stripping near (one-quarter of the virial radius, on average) the cluster center.