LeMMINGs - IV. The X-ray properties of a statistically complete sample of the nuclei in active and inactive galaxies from the Palomar sample

被引：15

作者：

Williams, D. R. A. ^{[1
,2
,3
]}

Pahari, M. ^{[3
,4
]}

Baldi, R. D. ^{[3
,5
]}

McHardy, I. M. ^{[3
]}

Mathur, S. ^{[6
,7
,8
]}

Beswick, R. J. ^{[1
]}

Beri, A. ^{[3
,9
]}

Boorman, P. ^{[10
]}

Aalto, S. ^{[11
]}

Alberdi, A. ^{[12
]}

Argo, M. K. ^{[13
]}

Dullo, B. T. ^{[14
]}

Fenech, D. M. ^{[15
]}

Green, D. A. ^{[15
]}

Knapen, J. H. ^{[16
,17
]}

Marti-Vidal, I ^{[18
,19
]}

Moldon, J. ^{[1
,12
]}

Mundell, C. G. ^{[20
]}

Muxlow, T. W. B. ^{[1
]}

Panessa, F. ^{[21
]}

Perez-Torres, M. ^{[12
]}

Saikia, P. ^{[22
]}

Shankar, F. ^{[3
]}

Stevens, I. R. ^{[23
]}

Uttley, P. ^{[24
]}

机构：

[1] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[2] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[3] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[4] Indian Inst Technol, Dept Phys, Hyderabad 502285, India

[5] INAF Ist Radioastron, Via P Gobetti 101, I-40129 Bologna, Italy

[6] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

[7] Ohio State Univ, Ctr Astron & Astroparticle Phys, Columbus, OH 43210 USA

[8] Eureka Sci, 2452 DELMER ST STE 100, Oakland, CA 94602 USA

[9] Indian Inst Sci Educ & Res IISER, DST INSPIRE Fac, Mohali 140306, Punjab, India

[10] Acad Sci, Astron Inst, Bocni 2 1401, CZ-14131 Prague, Czech Republic

[11] Chalmers Univ Technol, Dept Space Earth & Environm, Onsala Observ, SE-43992 Onsala, Sweden

[12] Inst Astrofis Andaluc IAA CSIC, Glorieta Astron S-N, E-18008 Granada, Spain

[13] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

[14] Univ Complutense Madrid, Dept Sica Tierra & Astrofis, IPARCOS, E-28040 Madrid, Spain

[15] Cavendish Lab, Astrophys Grp, 19 JJ Thomson Ave, Cambridge CB3 0HE, England

[16] Inst Astrofis Canarias, Via Lactea S-N, E-38205 San Cristobal la Laguna, Spain

[17] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Spain

[18] Univ Valencia, Observ Astron, Pare Cient, Valencia 46980, Spain

[19] Univ Valencia, Dept Astron & Astrofis, Valencia 46100, Spain

[20] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England

[21] INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy

[22] New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, POB 129188, Abu Dhabi, U Arab Emirates

[23] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

[24] Univ Amsterdam, Anton Pannekoek Inst Astron API, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2022年 / 510卷 / 04期

基金：

欧洲研究理事会;

关键词：

X-rays: galaxies; galaxies: active; DWARF SEYFERT NUCLEI; BLACK-HOLE MASS; GALACTIC NUCLEI; FUNDAMENTAL PLANE; RADIO-EMISSION; LUMINOSITY FUNCTION; LOCAL UNIVERSE; ACCRETION; SEARCH; SPECTRA;

D O I：

10.1093/mnras/stab3310

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

All 280 of the statistically complete Palomar sample of nearby (<120 Mpc) galaxies delta > 20 degrees have been observed at 1.5 GHz as part of the LeMMINGs e-MERLIN legacy survey. IIere, we present Chandra X-ray observations of the nuclei of 213 of these galaxies, including a statistically complete sub-set of 113 galaxies in the declination range 40 degrees <delta < 65 degrees. We observed galaxies of all optical spectral types, including 'active' galaxies [e.g. low-ionization nuclear emission line regions (LINERs) and Seyferts] and 'inactive' galaxies like H II galaxies and absorption line galaxies (ALG). The X-ray flux limit of our survey is 1.65 x 10(-14) erg s(-1) cm(-2) (0.3-10 keV). We detect X-ray emission coincident within 2 arcsec of the nucleus in 150/213 galaxies, including 13/14 Seyferts, 68/77 LINERs, 13/22 ALGs and 56/100 H II galaxies, but cannot completely rule out contamination from non-AGN processes in sources with nuclear luminosities less than or similar to 10(39) erg s(-1). We construct an X-ray Luminosity function (XI,F) and find that the local galaxy XLF, when including all active galactic nucleus (AGN) types, can be represented as a single power law of slope -0.54 +/- 0.06. The Eddington ratio of the Seyferts is usually 2-4 decades higher than that of the LINERs, ALGs, and H II galaxies, which are mostly detected with Eddington ratios less than or similar to 10(-3). Using [O III] line measurements and black hole masses from the literature, we show that LINERs, H II galaxies and ALGs follow similar correlations to low luminosities, suggesting that some 'inactive' galaxies may harbour AGN.

引用

页码：4909 / 4928

页数：20