J/MNRAS/440/2265 Spectroscopy of NGC3310 HII regions (Miralles-Caballero+, 2014)
Ionizing stellar population in the disc of NGC 3310.
I. The impact of a minor merger on galaxy evolution.
Miralles-Caballero D., Diaz A.I., Rosales-Ortega F.F., Perez-Montero E.,
Sanchez S.F.
<Mon. Not. R. Astron. Soc., 440, 2265-2289 (2014)>
=2014MNRAS.440.2265M 2014MNRAS.440.2265M
ADC_Keywords: Galaxies, nearby ; H II regions ; Spectroscopy
Keywords: techniques: spectroscopic - ISM: abundances - HII regions -
galaxies: evolution - galaxies: starburst - galaxies: stellar content
Abstract:
Numerical simulations of minor mergers predict little enhancement in
the global star formation activity. However, it is still unclear the
impact they have on the chemical state of the whole galaxy and on the
mass build-up in the galaxy bulge and disc. We present a
two-dimensional analysis of NCG 3310, currently undergoing an intense
starburst likely caused by a recent minor interaction, using data from
the PPAK Integral Field Spectroscopy Nearby Galaxies Survey (PINGS).
With data from a large sample of about a hundred HII regions
identified throughout the disc and spiral arms, we derive, using
strong-line metallicity indicators and direct derivations, a rather
flat gaseous abundance gradient. Thus, metal mixing processes
occurred, as in observed galaxy interactions. Spectra from PINGS data
and additional multiwavelength imaging were used to perform a spectral
energy distribution fitting to the stellar emission and a
photoionization modelling of the nebulae. The ionizing stellar
population is characterized by single populations with a narrow age
range (2.5-5Myr) and a broad range of masses (104-6x106M☉).
The effect of dust grains in the nebulae is important, indicating that
25-70% of the ultraviolet photons can be absorbed by dust. The
ionizing stellar population within the Hii regions represents
typically a few per cent of the total stellar mass. This ratio, a
proxy to the specific star formation rate, presents a flat or negative
radial gradient. Therefore, minor interactions may indeed play an
important role in the mass build-up of the bulge.
Description:
NGC 3310 observations were carried out with the 3.5m telescope of the
Calar Alto Observatory using the Postdam Multi-Aperture Spectrograph
(PMAS) in the PMAS fibre package mode (PPAK). This was part of the
PINGS (Rosales-Ortega et al., 2010MNRAS.405..735R 2010MNRAS.405..735R).
We retrieved publicly available broad-band imaging of this galaxy in
order to perform an absolute flux re-calibration. Specifically, we
used the Sloan Digital Sky Survey (SDSS, http://www.sdss.org/)
broad-band g- and r-filter images (with a spatial resolution of about
1-arcsec) and an HST (http://www.stsci.edu/hst/) image taken with the
Wide Field Planetary Camera 2 (WFPC2, with a spatial resolution of
about 0.05-arcsec) using the F439W filter (similar to B Johnson).
We also obtained UV images of the galaxy. In particular, taken with
the UVW2 and UVM2 filters (with effective wavelengths of 2087 and
2297Å, respectively), mounted on the OM camera on board the
XMM-Newton satellite.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 141 99 Catalogue of HII regions and reddening corrected
derived line intensities
tablea2.dat 132 29 Catalogue of external fibres and reddening
corrected derived line intensities
tablea3.dat 164 99 Properties of the HII regions derived via
χ2 minimization + CLOUDY analysis
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See also:
J/MNRAS/402/1005 : Stellar cluster dynamical masses in NGC3310 (Hagele+, 2010)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/99] HII region sequential number
4- 9 F6.2 arcsec DRA [-55/61] Relative right ascension (G1)
11- 16 F6.2 arcsec DDE [-79/64] Relative declination (G1)
18- 22 F5.2 arcsec Dist [0/95] Deprojected distance
24- 28 F5.1 --- [OII] Line intensity of [OII]3727,3729 (G2)
30- 33 F4.1 --- e_[OII] rms uncertainty on [OII]
35- 38 F4.1 --- Hg ?=- Line intensity of Hγ (G2)
40- 42 F3.1 --- e_Hg ? rms uncertainty on Hg
44- 48 F5.1 --- Hb [100] Line intensity of Hβ
50- 52 F3.1 --- e_Hb rms uncertainty on Hb
54- 58 F5.1 --- [OIII]1 Line intensity of [OIII]4959 (G2)
60- 63 F4.1 --- e_[OIII]1 rms uncertainty on [OIII]1
65- 69 F5.1 --- [OIII]2 Line intensity of [OIII]5007 (G2)
71- 74 F4.1 --- e_[OIII]2 rms uncertainty on [OIII]2
76- 79 F4.1 --- [NII]1 ?=- Line intensity of [NII]6548 (G2)
81- 83 F3.1 --- e_[NII]1 ? rms uncertainty on [NII]1
85- 89 F5.1 --- Ha Line intensity of Hα (2)
91- 94 F4.1 --- e_Ha rms uncertainty on Ha
96-100 F5.1 --- [NII]2 Line intensity of [NII]6584 (G2)
102-105 F4.1 --- e_[NII]2 rms uncertainty on [NII]2
107-110 F4.1 --- [SII]1 Line intensity of [SII]6717 (G2)
112-115 F4.1 --- e_[SII]1 rms uncertainty on [NII]1
117-120 F4.1 --- [SII]2 Line intensity of [SII]6731 (G2)
122-125 F4.2 --- e_[SII]2 rms uncertainty on [NII]2
126-131 F6.2 [mW/m2] logI(Hb) Hβ intensity (erg/cm2/s)
133-136 F4.2 --- c(Hb) [0/0.3] Extinction coefficient
138-141 F4.2 --- e_c(Hb) [0/0.04]? rms uncertainty on c(Hb)
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Note (2): in a few cases, Ha/Hb is less than the theoretical adopted ratio of
2.87, even within errors. However, systematics, of the order of 10% for this
ratio, are not included in the reported uncertainties
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/29] External region sequential number
4- 9 F6.2 arcsec DRA Relative right ascension (G1)
11- 17 F7.2 arcsec DDE Relative declination (G1)
19- 24 F6.2 arcsec Dist Deprojected distance
26- 31 F6.1 --- [OII] Line intensity of [OII]3727,3729 (G2)
33- 37 F5.1 --- e_[OII] rms uncertainty on [OII]
39- 43 F5.1 --- Hb [100] Line intensity of Hβ
45- 47 F3.1 --- e_Hb rms uncertainty on Hb
49- 53 F5.1 --- [OIII]1 Line intensity of [OIII]4959 (G2)
55- 57 F3.1 --- e_[OIII]1 rms uncertainty on [OIII]1
59- 63 F5.1 --- [OIII]2 Line intensity of [OIII]5007 (G2)
65- 68 F4.1 --- e_[OIII]2 rms uncertainty on [OIII]2
70- 73 F4.1 --- [NII]1 Line intensity of [NII]6548 (G2)
75- 77 F3.1 --- e_[NII]1 rms uncertainty on [NII]1
79- 83 F5.1 --- Ha Line intensity of Hα (G2)
85- 88 F4.1 --- e_Ha rms uncertainty on Ha
90- 93 F4.1 --- [NII]2 Line intensity of [NII]6584 (G2)
95- 97 F3.1 --- e_[NII]2 rms uncertainty on [NII]2
99-102 F4.1 --- [SII]1 Line intensity of [SII]6717 (G2)
104-106 F3.1 --- e_[SII]1 rms uncertainty on [NII]1
108-111 F4.1 --- [SII]2 Line intensity of [SII]6731 (G2)
113-115 F3.1 --- e_[SII]2 rms uncertainty on [NII]2
117-122 F6.2 [mW/m2] logI(Hb) Hβ intensity
124-127 F4.2 --- c(Hb) Extinction coefficient
129-132 F4.2 --- e_c(Hb) ? rms uncertainty on c(Hb)
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/99] HII region sequential number
4- 8 F5.1 aW/m2/nm FUVW2 Observed flux density through XMM-OT UVW2
filter (1)
10- 13 F4.1 aW/m2/nm e_FUVW2 rms uncertainty on FUVW2
15- 19 F5.1 aW/m2/nm FUVM2 ?=- Observed flux density through XMM-OT UVM2
filter (1)
21- 24 F4.1 aW/m2/nm e_FUVM2 ? rms uncertainty on FUVM2
26- 29 F4.1 aW/m2/nm Fu ?=- Observed flux density through SDSS u
filter (1)
31- 34 F4.1 aW/m2/nm e_Fu ? rms uncertainty on Fu
36- 40 F5.2 aW/m2/nm FF439W Observed flux density through HST/WFPC2 F439W
filter (1)
42- 46 F5.2 aW/m2/nm e_FF439W rms uncertainty on FF439W
48- 53 F6.2 aW/m2/nm FF547M Observed flux density through HST/WFPC2 F547M
filter (1)
55- 58 F4.2 aW/m2/nm e_FF547M rms uncertainty on FF547M
60- 65 F6.2 aW/m2/nm FF621M Observed flux density through HST/WFPC2 F621M
filter (1)
67- 70 F4.2 aW/m2/nm e_FF621M rms uncertainty on FF621M
72- 77 F6.2 aW/m2/nm Fi ?=- Observed flux density through SDSS i
filter (1)
79- 82 F4.2 aW/m2/nm e_Fi ? rms uncertainty on Fi
84- 88 F5.2 aW/m2/nm Fz ?=- Observed flux density through SDSS z
filter (1)
90- 93 F4.2 aW/m2/nm e_Fz ? rms uncertainty on Fz
95- 98 I4 0.1nm EWHa ?=- Derived Hα equivalent width (1)
100-102 I3 0.1nm e_EWHa ? rms uncertainty on EWHa
104-106 I3 0.1nm EWHb ?=- Derived Hβ equivalent width (1)
108-109 I2 0.1nm e_EWHb ? rms uncertainty on EWHb
111-114 F4.2 [yr] logtau Derived age of the ionizing population
116-119 F4.2 [yr] E_logtau ? Error on logtau (upper value)
121-124 F4.2 [yr] e_logtau ? Error on logtau (lower value)
126-129 F4.2 [Msun] logMion Derived mass of the ionizing population
131-134 F4.2 [Msun] E_logMion ? Error on logMion (upper value)
136-139 F4.2 [Msun] e_logMion ? Error on logMion (lower value)
141-144 F4.2 mag AV Derived internal extinction
146-149 F4.2 mag E_AV ? Error on AV (upper value)
151-154 F4.2 mag e_AV ? Error on AV (lower value)
156-158 F3.1 --- fd [1/3.9] Derived absorption factor due to
dust grain within the nebulae
160-163 F4.2 --- e_fd ? rms uncertainty on fd
164 A1 --- f_fd [:] : indicated fixed value of fd to 1 (3)
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Note (1): corrected by the emission of the non-ionizing population, in
10-16erg/cm2/s/Å.
Note (3): In those cases where no error is reported in the derived properties
of the HII regions, a successful fit was not achieved and only those derived
values for the minimum computed chi2 are shown.
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Global notes:
Note (G1): with respect to the center of the galaxy (HII region ID 3,
[HDC2010] N of Hagele et al., 2010, Cat. J/MNRAS/402/1005) located
at position 10:38:45.893+53:30:11.47 (J2000).
Note (G2): all intensities are normalized to Hβ=100
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 27-Jan-2015