J/other/RAA/14.1393 HII regions in interacting system Arp 86 (Zhou+, 2014)
Metallicity and star formation activities of the interacting system Arp 86 from
observations with MOS on the Xinglong 2.16m telescope.
Zhou Z.-M., Wu H., Huang L., Li H.-B., Zhou Z.-Z., Jia J.-J., Lam M.-I.,
Zhu Y.-N.
<Res. Astron. Astrophys., 14, 1393-1405 (2014)>
=2014RAA....14.1393Z 2014RAA....14.1393Z
ADC_Keywords: Galaxies, nearby ; H II regions ; Spectroscopy
Keywords: galaxies: abundances - galaxies: evolution - galaxies: interactions -
(ISM:) H II regions - techniques: spectroscopic
Abstract:
We present an analysis of the metallicity and star formation
activities of HII regions in the interacting system Arp 86, based on
the first scientific observations using multi-object spectroscopy with
the 2.16m telescope at the Xinglong Observing Station. We find that
the oxygen abundance gradient in Arp 86 is flatter than that in normal
disk galaxies, which confirms that gas inflows caused by tidal forces
during encounters can flatten the metallicity distributions in
galaxies. The companion galaxy NGC 7752 is currently experiencing a
galaxy-wide starburst with a higher star formation rate surface
density than the main galaxy NGC 7753, which can be explained in that
the companion galaxy is more susceptible to the effects of interaction
than the primary. We also find that the galaxy 2MASX J23470758+2926531
has similar abundance and star formation properties to NGC 7753, and
may be a part of the Arp 86 system.
Description:
We obtained optical spectroscopy of HII region candidates with the
MOS at the f/9 Cassegrain focus of the Xinglong 2.16m telescope. Our
observations were carried out on the nights of 2012 September 15-17,
using four multi-object masks with apertures of 2.7" in diameter.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 124 70 Sample of observed HII regions
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [1/70] HII region sequential number
4- 5 I2 h RAh Right ascension (J2000)
7- 8 I2 min RAm Right ascension (J2000)
10- 14 F5.2 s RAs Right ascension (J2000)
16 A1 --- DE- Declination sign (J2000)
17- 18 I2 deg DEd Declination (J2000)
20- 21 I2 arcmin DEm Declination (J2000)
23- 27 F5.2 arcsec DEs Declination (J2000)
29- 36 F8.2 0.1aW/m2 F[OII] ?=- Line flux of [OII]3727 (1)
38- 44 F7.2 0.1aW/m2 e_F[OII] ? rms uncertainty on F[OII]
47- 52 F6.2 0.1aW/m2 F[OIII] ?=- Line flux of [OIII]5007 (1)
54- 59 F6.2 0.1aW/m2 e_F[OIII] ? rms uncertainty on F[OIII]
62- 69 F8.3 0.1aW/m2 FHa Line flux of Hα (1)
71- 76 F6.3 0.1aW/m2 e_FHa rms uncertainty on FHa
79- 86 F8.3 0.1aW/m2 F[NII] Line flux of [NII]6583 (1)
88- 93 F6.3 0.1aW/m2 e_F[NII] rms uncertainty on F[NII]
96-101 F6.2 0.1aW/m2 F[SII] Line flux of [SII]6717,6731 (1)
103-107 F5.2 0.1aW/m2 e_F[SII] rms uncertainty on F[SII]
110-113 F4.2 --- c(Hb) ?=- logarithmic extinction at Hβ)
115-118 F4.2 --- Abund Abundance, 12+log(O/H)
120-124 F5.2 [Msun/yr] logSFR Star formation rate
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Note (1): in 10-16erg/cm2/s, after correcting for reddening and extinction.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 30-Apr-2015