MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

Shimakawa, Rhythm; Koyama, Yusei; Röttgering, Huub J. A.; Kodama, Tadayuki; Hayashi, Masao; Hatch, Nina A.; Dannerbauer, Helmut; Tanaka, Ichi; Tadaki, Ken-ichi; Suzuki, Tomoko L. et al.
Referencia bibliográfica

Monthly Notices of the Royal Astronomical Society, Volume 481, Issue 4, p.5630-5650

Fecha de publicación:
12
2018
Descripción
This paper is the second in a series presenting the results of our deep H α-line survey towards protoclusters at z > 2, based on narrow-band imaging with the Subaru Telescope. This work investigates massive galaxies in a protocluster region associated with a radio galaxy (PKS 1138 - 262), the Spiderweb galaxy, at z = 2.2. Our 0.5 mag deeper narrow-band imaging than previous surveys collects a total of 68 H α emitters (HAE). Here, 17 out of the 68 are newly discovered protocluster members. First, a very high characteristic stellar mass of M_\star ^\ast = 10^{11.73} M⊙ is measured from a Schechter function fit to the mass distribution of HAEs. Together with the Chandra X-ray data, we find that four out of six massive HAEs (M⋆ > 1011 M⊙) show bright X-ray emission, suggesting that they host active galactic nuclei (AGNs). Their mass estimates, therefore, would be affected by the nuclear emission from AGNs. Notably, the X-ray-detected HAEs are likely positioned near the boundary between star-forming and quiescent populations in the rest-frame UVJ plane. Moreover, our deep narrow-band data succeed in probing the bright H α (+ [N II]) line nebula of the Spiderweb galaxy extending over ˜100 physical kpc. These results suggest that the massive galaxies in the Spiderweb protocluster are on the way to becoming the bright red sequence objects seen in local galaxy clusters, where AGNs might play an essential role in their quenching processes, though a more statistical database is needed to build a general picture.
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Dos cuestiones fundamentales en la Astrofísica son la conversión de gas molecuar en estrellas y cómo este proceso físico depende del entorno en todas las escalas, desde sistemas planetarios, cúmulos estelares, galaxias hasta cúmulos de galaxias. El objectivo principal de este proyecto es el de estudiar la formación y evolución de galaxias a partir

Helmut
Dannerbauer