Lyα view around a z = 2.84 hyperluminous QSO at a node of the cosmic web

PASJ: Publications of the Astronomical Society of Japan

Hayashino, Tomoki¹  Kikuta, Satoshi²  Saito, Tomoki²  Cen, Renyue²  Yagi, Masafumi³  Komiyama, Yutaka⁴  Steidel, Charles C⁵  Imanishi, Masatoshi⁵  Matsuda, Yuichi⁵  Momose, Rieko⁶ 

[1] Cahill Center for Astronomy and Astrophysics, California Institute of Technology, MS 249-17, Pasadena, CA 91125, USA;Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan;Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA;Graduate School of Science and Engineering, Hosei University, 3-7-2 Kajino-cho, Koganei, Tokyo 184-8584, Japan;National Astronomical Observatory of Japan (NAOJ), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan;Research Center for Neutrino Science, Tohoku University, Aramaki, Aoba-ku, Sendai, Miyagi 980-8578, Japan

关键词: galaxies: formation;    (galaxies:) intergalactic medium;    galaxies: high-redshift;    (galaxies:) quasars: individual;   

DOI  :  10.1093/pasj/psz055

学科分类：天文学(综合)

来源: Oxford University Press

【 摘 要 】

We report on the results of deep and wide-field (1.1 deg2) narrow-band observations with Subaru/Hyper Suprime-Cam (HSC) of a field around a hyperluminous QSO (HLQSO), HS|$\, 1549+$|1919, residing in a protocluster at z = 2.84, to map the large-scale structure of Lyα emitters (LAEs). One HSC pointing enables us to detect 3490 LAEs and 76 extended Lyα blobs (LABs), probing diverse environments from voids to protoclusters. The HLQSO is found to be near the center of the protocluster, which corresponds to the intersection of |$\sim \,$|100 comoving Mpc-scale structures of LAEs. LABs are basically distributed along the large-scale structure, with larger ones particularly clustering around the HLQSO, confirming a previously noted tendency of LABs to prefer denser environments. Moreover, the shapes of LABs near the HLQSO appear to be aligned with the large-scale structure. Finally, a deep Lyα image reveals a diffuse Lyα nebula along a filamentary structure with no luminous UV/sub-mm counterpart. We suggest that the diffuse nebula is due to a cold filament with high clumping factor illuminated by the QSO, with the required high clumpiness provided by unresolved residing halos of mass |$\le 10^{9-10}\, M_\odot$|⁠.

【 授权许可】

CC BY