J/A+A/666/A29 M83 PNe in MUSE+HST dataset (Della+, 2022)
Stellar feedback in M 83 as observed with MUSE. II.
Analysis of the H II region population: Ionisation budget and pre-SN feedback.
Della Bruna L., Adamo A., McLeod A.F., Smith L.J., Savard G., Robert C.,
Sun J., Amram P., Bik A., Blair W.P., Long K.S., Renaud F., Walterbos R.,
Usher C.
<Astron. Astrophys., 666, A29 (2022)>
=2022A&A...666A..29D 2022A&A...666A..29D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Planetary nebulae ; Positional data ; Optical
Keywords: galaxies: star clusters: general
Abstract:
Energy and momentum injected by young, massive stars into the
surrounding gas play an important role in regulating further star
formation and in determining the galaxy's global properties. Before
supernovae begin to explode, stellar feedback consists of two main
processes: radiation pressure and photoionisation.
We study pre-supernova feedback and constrain the leakage of Lyman
continuum (LyC) radiation in a sample of ∼4700 HII regions in the
nearby spiral galaxy M 83. We explore the impact that the galactic
environment and intrinsic physical properties (metallicity,
extinction, and stellar content) have on the early phases of HII
region evolution.
We combined VLT/MUSE observations of the ionised gas with young star
cluster physical properties derived from HST multiwavelength data. We
identified HII regions based on their Hα emission, and
cross-matched the sample with planetary nebulae and supernova remnants
to assess contaminant sources and identify evolved HII regions. We
also spectroscopically identified Wolf-Rayet (WR) stars populating the
star-forming regions. We estimated the physical properties of the HII
regions (luminosity, size, oxygen abundance, and electron density).
For each HII region, we computed the pressure of ionised gas (Pion)
and the direct radiation pressure (Pdir) acting in the region, and
investigated how they vary with galactocentric distance, with the
physical properties of the region, and with the pressure of the
galactic environment (PDE). For a subset of ∼500 regions, we
also investigated the link between the pressure terms and the
properties of the cluster population (age, mass, and LyC flux). By
comparing the LyC flux derived from Hα emission with the one
modelled from their clusters and WRs, we furthermore constrained any
escape of LyC radiation (fesc).
We find that Pion dominates over Pdir by at least a factor of 10
on average over the disk. Both pressure terms are strongly enhanced
and become almost comparable in the central starburst region. In the
disk (R >= 0.15 Re), we observe that Pdir stays approximately
constant with galactocentric distance. We note that Pdir is
positively correlated with an increase in radiation field strength
(linked to the negative metallicity gradient in the galaxy), while it
decreases in low extinction regions, as is expected if the amount of
dust to which the momentum can be imparted decreases. In addition,
Pion decreases constantly for increasing galactocentric distances;
this trend correlates with the decrease in extinction - indicative of
more evolved and thus less compact regions - and with changes in the
galactic environment (traced by a decrease in PDE). In general, we
observe that HII regions near the centre are underpressured with
respect to their surroundings, whereas regions in the rest of the disk
are overpressured and hence expanding. We find that regions hosting
younger clusters or those that have more mass in young star clusters
have a higher internal pressure, indicating that clustered star
formation likely plays a dominant role in setting the pressure.
Finally, we estimate that only 13% of HII regions hosting young
clusters and WR stars have fesc≥0, which suggests that star
formation taking place outside young clusters makes a non-negligible
contribution to ionising HII regions.
Description:
The position and coordinates of the 120 confirmed PNe can be found in
Table B.1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 43 244 Coordinates of the PNe identified in the
MUSE+HST dataset
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See also:
J/ApJ/703/894 : PNe in 5 nearby galaxies (Herrmann+, 2009)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Name PN Name, PNnnn
8- 9 I2 h RAh Right ascension (J2000)
11- 12 I2 min RAm Right ascension (J2000)
14- 19 F6.3 s RAs Right ascension (J2000)
21 A1 --- DE- Declinaiton sign (J2000)
22- 23 I2 deg DEd Declinaiton (J2000)
25- 26 I2 arcmin DEm Declinaiton (J2000)
28- 33 F6.3 arcsec DEs Declinaiton (J2000)
35 I1 --- Class [1/3] Class code (1)
37- 43 A7 --- HC2009b Herrmann & Ciardullo (2009ApJ...703..894H 2009ApJ...703..894H,
Cat. J/ApJ/703/894) cross reference,
M83-NNN ([HC2009b] M83-NNN in Simbad)
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Note (1): Classification score as follows:
1 = spectroscopically confirmed
2 = spectroscopically confirmed with additional HeII4686 detection
3 = candidate (visually identified)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 20-Feb-2023