prikaz prve stranice dokumenta The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field
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Scientific paper - Original scientific paper
The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field
Monthly Notices of the Royal Astronomical Society, 474 (2018), 3; 4133-4150. https://doi.org/10.1093/mnras/stx2954
Hale, C. L.; Jarvis, M. J.; Delvecchio, I.; Hatfield, P. W.; Novak, Mladen; Smolčić, Vernesa; Zamorani, G.

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Hale, C. L., Jarvis, M. J., Delvecchio, I., Hatfield, P. W., Novak, M., Smolčić, V. & Zamorani, G. (2018). The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field. Monthly Notices of the Royal Astronomical Society, 474. (3), 4133-4150. doi: 10.1093/mnras/stx2954

Hale, C. L., et al. "The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field." Monthly Notices of the Royal Astronomical Society, vol. 474, no. 3, 2018, pp. 4133-4150. https://doi.org/10.1093/mnras/stx2954

Hale, C. L., M. J. Jarvis, I. Delvecchio, P. W. Hatfield, Mladen Novak, Vernesa Smolčić and G. Zamorani. "The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field." Monthly Notices of the Royal Astronomical Society 474, no. 3 (2018): 4133-4150. https://doi.org/10.1093/mnras/stx2954

Hale, C. L., et al. (2018) 'The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field', Monthly Notices of the Royal Astronomical Society, 474(3), pp. 4133-4150. doi: 10.1093/mnras/stx2954

Hale CL, Jarvis MJ, Delvecchio I, Hatfield PW, Novak M, Smolčić V, and sur.. The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field. Monthly Notices of the Royal Astronomical Society [Internet]. 2018 [cited 2024 December 19];474(3):4133-4150. doi: 10.1093/mnras/stx2954

C. L. Hale, et al., "The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field", Monthly Notices of the Royal Astronomical Society, vol. 474, no. 3, pp. 4133-4150, 2018. [Online]. Available at: https://urn.nsk.hr/urn:nbn:hr:217:807218. [Accessed: 19 December 2024]

Metadata
Title (english)The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field
AuthorC. L. Hale
AuthorM. J. Jarvis
AuthorI. Delvecchio
AuthorP. W. Hatfield
AuthorMladen Novak
MBZ: 344074
AuthorVernesa Smolčić
MBZ: 336180
AuthorG. Zamorani
Author's institutionUniversity of Zagreb
Faculty of Science
(Department of Physics)
Scientific / art field,
discipline and subdiscipline		NATURAL SCIENCES
Physics
Astronomy and Astrophysics
Abstract (english)
Dark matter haloes in which galaxies reside are likely to have a significant impact on their evolution. We investigate the link between dark matter haloes and their constituent galaxies by measuring the angular two-point correlation function of radio sources, using recently released 3 GHz imaging over ∼2 deg2 of the Cosmological Evolution Survey (COSMOS) field. We split the radio source population into star-forming galaxies (SFGs) and active galactic nuclei (AGN), and further separate the AGN into radiatively efficient and inefficient accreters. Restricting our analysis to z < 1, we find SFGs have a bias, b = 1.5+0.1 −0.2, at a median redshift of z = 0.62. On the other hand, AGN are significantly more strongly clustered with b = 2.1 ± 0.2 at a median redshift of 0.7. This supports the idea that AGN are hosted by more massive haloes than SFGs. We also find low accretion rate AGN are more clustered (b = 2.9 ± 0.3) than high accretion rate AGN (b = 1.8+0.4 −0.5) at the same redshift (z ∼ 0.7), suggesting that low accretion rate AGN reside in higher mass haloes. This supports previous evidence that the relatively hot gas that inhabits the most massive haloes is unable to be easily accreted by the central AGN, causing them to be inefficient. We also find evidence that low accretion rate AGN appear to reside in halo masses of Mh ∼ 3–4 × 1013 h−1 M at all redshifts. On the other hand, the efficient accreters reside in haloes of Mh ∼ 1–2 × 1013 h−1 M at low redshift but can reside in relatively lower mass haloes at higher redshifts. This could be due to the increased prevalence of cold gas in lower mass haloes at z ≥ 1 compared to z < 1.
Keywords (english)
Languageenglish
Publication typeScientific paper - Original scientific paper
Publication statusPublished
Peer reviewPeer review - international
Publication versionPublished version
Journal titleMonthly Notices of the Royal Astronomical Society
Numberingvol. 474, no. 3, pp. 4133-4150
p-ISSN0035-8711
e-ISSN1365-2966
DOIhttps://doi.org/10.1093/mnras/stx2954
URN:NBNurn:nbn:hr:217:807218
Publication2018
Document URLhttps://academic.oup.com/mnras/article/474/3/4133/4643178
Type of resourceText
Access conditionsOpen access
Terms of useLicence In copyright icon
Public note© 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 November 13. Received 2017 November 7; in original form 2017 May 12.
Created on2020-03-01 11:34:51