2022PASJ...74.1356T

Query : 2022PASJ...74.1356T

2022PASJ...74.1356T - Publ. Astron. Soc. Jap., 74, 1356-1367 (2022/December-6)

Optical IFU observations of GOALS sample with KOOLS-IFU on Seimei Telescope: Initial results of nine U/LIRGs at z < 0.04.

TOBA Y., YAMADA S., MATSUBAYASHI K., TERAO K., MORIYA A., UEDA Y., OHTA K., HASHIGUCHI A., HIMOTO K.G., IZUMIURA H., JOH K., KATO N., KOYAMA S., MAEHARA H., MISATO R., NOBORIGUCHI A., OGAWA S., OTA N., SHIBATA M., TAMADA N., YANAGAWA A., YONEKURA N., NAGAO T., AKIYAMA M., KAJISAWA M. and MATSUOKA Y.

Abstract (from CDS):

We present ionized gas properties of nine local ultra/luminous infrared galaxies (U/LIRGs) at z < 0.04 through Integral Field Unit (IFU) observations with KOOLS-IFU on the Seimei Telescope. The observed targets are drawn from the Great Observatories All-sky LIRG Survey (GOALS), covering a wide range of merger stages. We successfully detect emission lines such as Hβ, [O III]λ5007, Hα, [N II]λλ6549, 6583, and [S II]λλ6717, 6731 with a spectral resolution of R = 1500-2000, which provides (i) a spatially resolved (∼200-700 pc) moment map of ionized gas and (ii) diagnostics for an active galactic nucleus (AGN) within the central ∼3-11 kpc in diameter for our sample. We find that the [O III] outflow that is expected to be driven by an AGN tends to be stronger (i) towards the galactic center and (ii) as a sequence of the merger stage. In particular, the outflow strength in the late-stage (stage D) mergers is about 1.5 times stronger than that in the early-state (stage B) mergers, which indicates that galaxy mergers could induce AGN-driven outflow and play an important role in the co-evolution of galaxies and supermassive black holes.

Abstract Copyright: © The Author(s) 2022. Published by Oxford University Press on behalf of the Astronomical Society of Japan.

Journal keyword(s): galaxies: active - infrared: galaxies - methods: observational

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * 29 Psc V* 00 01 49.4481127032 -03 01 39.011820024 4.47 4.98 5.10     B7III-IV 232 0
2 * ksi02 Cet * 02 28 09.5570589539 +08 27 36.216809306 4.14 4.25 4.30 4.29 4.34 B9III 352 0
3 NGC 1614 Sy1 04 34 00.027 -08 34 44.57   14.66 13.99     ~ 697 1
4 BD+52 913 WD* 05 05 30.6180977592 +52 49 51.919301604 10.25 11.44 11.69 11.93 12.108 DA.8 1153 0
5 Z 468-2 Sy2 05 08 19.7062775592 +17 21 48.085162020   15.4       ~ 129 0
6 * eta Hya bC* 08 43 13.4757536071 +03 23 55.182801587 3.380 4.100 4.300 4.37 4.56 B3V 418 1
7 NGC 3690 IG 11 28 31.0 +58 33 41   13.19 12.86     ~ 1015 4
8 NGC 3690B GiP 11 28 31.02 +58 33 40.7   11.8       ~ 635 4
9 NGC 3690NE AGN 11 28 33.07 +58 33 54.2   11.8       ~ 635 4
10 HZ 43A WD* 13 16 21.8532409720 +29 05 55.411186877   12.52 12.66     DAwk 477 0
11 Z 271-60 Sy2 13 44 42.1883001099 +55 53 13.596220922   15.68 14.91     ~ 958 3
12 * 108 Vir * 14 45 30.2044637184 +00 43 02.180202816   5.656 5.665     B9.5V 165 0
13 NGC 6786 Sy2 19 10 53.928 +73 24 36.20   13.7       ~ 80 1
14 Z 341-20 G 19 11 04.67 +73 25 36.0   15.1       ~ 40 0
15 * 58 Aql * 19 54 44.7948526968 +00 16 25.050363384   5.703 5.631     B9IV 228 0
16 NGC 6921 Sy2 20 28 28.8658027224 +25 43 24.094324884 15.41   12.897     ~ 104 1
17 NGC 7674 Sy1 23 27 56.6973043968 +08 46 44.253707772 13.84 13.92 13.23 12.64   ~ 738 2
18 NGC 7679 Sy2 23 28 46.6613717400 +03 30 41.013578196   13.2       ~ 289 1

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