Bibcode
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.; Fukagawa, Nao; Cai, Zheng; Kurk, Jaron D.
Referencia bibliográfica
Monthly Notices of the Royal Astronomical Society, Volume 481, Issue 4, p.5630-5650
Advertised on:
12
2018
Número de citas
42
Número de citas referidas
39
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.
Proyectos relacionados
![Formación de un cúmulo de galaxies en el universo lejano, sus miembros están interactuando unas con otras y formando nuevas estrellas de forma muy activa. Crédito: ESO/M. Kornmesser. Proto-cúmulo de galaxias](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/project/Imagen%20Helmut.jpg?itok=HFiPhhs4)
Gas Molecular y Polvo en Galacias através del Tiempo Cósmico
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