J/MNRAS/511/6087 PNes and SNRs in nearby galaxies (Scheuermann+, 2022)
Planetary nebula luminosity function distances for 19 galaxies observed by
PHANGS-MUSE.
Scheuermann F., Kreckel K., Anand G.S., Blanc G.A., Congiu E., Santoro F.,
Van Dyk S.D., Barnes A.T., Bigiel F., Glover S.C.O., Groves B.,
Klessen R.S., Kruijssen J.M.D., Rosolowsky E., Schinnerer E., Schruba A.,
Watkins E.J., Williams T.G.
<Mon. Not. R. Astron. Soc. 511, 6087-6109 (2022)>
=2022MNRAS.511.6087S 2022MNRAS.511.6087S (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; Supernova remnants ; Galaxies, nearby ;
Galaxies, photometry ; Spectroscopy ; Optical ; Line Profiles ;
Positional data ; Magnitudes
Keywords: galaxies: distances and redshifts - ISM: supernova remnant -
planetary nebulae: general
Abstract:
We provide new planetary nebula luminosity function (PNLF) distances
to 19 nearby spiral galaxies that were observed with VLT/MUSE by the
PHANGS collaboration. Emission line ratios are used to separate
planetary nebulae (pne) from other bright [O III] emitting sources
like compact supernovae remnants (SNRS) or H II regions. While many
studies have used narrowband imaging for this purpose, the detailed
spectral line information provided by integral field unit (IFU)
spectroscopy grants a more robust way of categorizing different [O III]
emitters. We investigate the effects of snr contamination on the PNLF
and find that we would fail to classify all objects correctly, when
limited to the same data narrowband imaging provides. However, the few
misclassified objects usually do not fall on the bright end of the
luminosity function, and only in three cases does the distance change
by more than 1σ. We find generally good agreement with
literature values from other methods. Using metallicity constraints
that have also been derived from the same IFU data, we revisit the
pnlf zero-point calibration. Over a range of 8.34 < 12 + log(O/H) <
8.59, our sample is consistent with a constant zero- point and yields
a value of M* = -4.542+0.103_-0.059 mag, within 1σ of other
literature values. MUSE pushes the limits of PNLF studies and makes
galaxies beyond 20 Mpc accessible for this kind of analysis. This
approach to the PNLF shows great promise for leveraging existing
archival IFU data on nearby galaxies.
Description:
In our study, we use data that were observed PHANGS, a collaboration
aimed at studying the baryon cycle within galaxies at high spatial
resolution, sufficient to isolate and characterise individual
molecular clouds and H II regions. One of the pillars of this
project are optical IFU spectroscopy observations with the Multi Unit
Spectroscopic Explorer at the Very Large Telescope (VLT). The
PHANGS-MUSE sample consists of 19 nearby spiral galaxies that are all
roughly face-on. This paper has three objectives. The first aim is to
test how susceptible narrowband imaging is to misclassifying snrs as
pne. The second goal is to quantify the applicability of IFU surveys
for pn studies. Past pn studies required special observations that
were taken for the sole purpose of finding pne.Here we try to quantify
whether IFU surveys can compensate the smaller fields of view with a
gain in spectral information and explorer the limitations to derive
pnlf-based distances from IFU observations.The last objective is to
provide new and precise distance measurements for the 19 nearby
galaxies observed by the PHANGS-MUSE survey, some of which did not
have good distance estimates before, (i.e see section Introduction).
As explained along the section 2.1 Data, using this full 19 nearby
galaxies sample, data reduction was performed by the PHANGS-MUSE team,
using the MUSE data processing pipeline. They produced reduced and
mosaicked spectral cubes that form the base for further data analysis
pipeline (DAP) products which we use for our analysis. This includes
emission line maps that are extracted by fitting Gaussian profiles
along with the stellar continuum. Next (2.2 section), we proceed to
source detection and extraction lines photometry. Then, after aperture
and galactic extinction corrections on [O III], [N II], [S II] and
Hα, we are able to provide precise flux values as well as
precise positions and object types (PNe and SNR) presented in the
table2.dat (i.e see also the section 3 for details on PNe luminosity
function serving to retreive the 19 acurate galaxy distances).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
galaxy.dat 11 19 Nearby galaxies sample
table2.dat 202 1049 Our sample of 899 PNe across 19 nearby galaxies
observed for the PHANGS-MUSE program and 150 SNR
well flagged
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See also:
J/A+A/608/A2 : MUSE Hubble Ultra Deep Field Survey. II. (Inami+, 2017)
J/A+A/637/A62 : Fornax3D. Planetary nebulae automated detection
(Spriggs+, 2020)
J/ApJ/339/53 : Planetary nebulae as standard candles. II. (Ciardullo+, 1989)
J/ApJ/577/31 : PNe in six galaxies (Ciardullo+, 2002)
J/A+A/653/A167 : Fornax3D PNe Catalogue (Spriggs+, 2021)
J/ApJ/916/21 : OIII PN luminosity functions from MUSE datacubes (Roth+, 2021)
J/A+A/658/A188 : PHANGS-MUSE sample HII regions catalog (Santoro+, 2022)
Byte-by-byte Description of file: galaxy.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Galaxy Galaxy name (gal_name)
9- 11 I3 --- Nbr Number of PNe/SNR within the galaxy
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Galaxy Galaxy name (gal_name)
9- 11 I3 --- ID PNe/SNR identifier relative number in
their hosted galaxy (id)
13- 15 A3 --- Type Object type, 899 PNs and 150 SNRs in our
sample (type)
17- 18 I2 h RAh Right ascension (J2000)
20- 21 I2 min RAm Right ascension (J2000)
23- 27 F5.2 s RAs Right ascension (J2000)
29 A1 --- DE- Declination sign (J2000)
30- 31 I2 deg DEd Declination (J2000)
33- 34 I2 arcmin DEm Declination (J2000)
36- 40 F5.2 arcsec DEs Declination (J2000)
42- 57 F16.13 mag OIIImag Apparent aperture/extinction corrected
[O III] line magnitude (mOIII) (1)
59- 75 F17.15 mag e_OIIImag Estimated error of OIIImag (dmOIII)
77- 94 F18.15 [-] logOIII/Ha Logarithm of I_[O III]_ to IHα
fluxes ratio, with fluxes in erg/s/cm2
(logOIII/Ha)
96- 112 F17.15 [-] e_logOIII/Ha Estimated error of logOIII/Ha (dlogOIII/Ha)
114- 131 F18.15 [-] logNII/Ha Logarithm of I_[N II]_ to IHα
fluxes ratio (logNII/Ha)
133- 149 F17.15 [-] e_logNII/Ha Estimated error of logNII/Ha (dlogNII/Ha)
151- 168 F18.15 [-] logSII/Ha Logarithm of I_[S II]_ to IHα
fluxes ratio (logSII/Ha)
170- 186 F17.15 [-] e_logSII/Ha Estimated error of logSII/Ha (dlogSII/Ha)
188- 202 A15 --- Note Notes on objects (note) (2)
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Note (1): Converted with fluxes via equation 4 as -2.5.log10 I_[O III]_
-13.74 of the section 2.2 Source detection and photometry.
Note (2): OL means rejected as overluminous for 8 of our sources, the SNR
NGC3627-5 is also named Ciardullo-PN-35 and the SNR NGC3351-2 is also
named Ciardullo-PN-5.
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 06-Feb-2025