J/ApJS/271/40 PN LF distances using VLT-MUSE. II. Archival data (Jacoby+, 2024)
Toward precision cosmology with improved planetary nebula luminosity function
distances using VLT-MUSE.
II. A test sample from archival data.
Jacoby G.H., Ciardullo R., Roth M.M., Arnaboldi M., Weilbacher P.M.
<Astrophys. J. Suppl. Ser., 271, 40 (2024)>
=2024ApJS..271...40J 2024ApJS..271...40J
ADC_Keywords: Galaxies, nearby; Optical; Planetary nebulae; Magnitudes
Keywords: Galaxies ; Distance indicators ; Hubble constant ; Planetary nebulae
Abstract:
Thanks to the MUSE integral field spectrograph on board the Very Large
Telescope (VLT), extragalactic distance measurements with the
[OIII]λ5007 planetary nebula luminosity function (PNLF) are now
possible out to ∼40Mpc. Here we analyze the VLT/MUSE data for
20 galaxies from the ESO public archive to identify the systems'
planetary nebulae (PNe) and determine their PNLF distances. Three of
the galaxies do not contain enough PNe for a robust measure of the
PNLF, and the results for one other system are compromised of the
galaxy's internal extinction. However, we obtain robust PNLF distances
for the remaining 16 galaxies, two of which are isolated and beyond
30Mpc in a relatively unperturbed Hubble flow. From these data, we
derive a Hubble constant of 74.2±7.2(stat)±3.7(sys)km/s/Mpc, a
value that is very similar to that found from other quality indicators
(e.g., Cepheids, the tip of the red giant branch, and surface
brightness fluctuations). At present, the uncertainty is dominated by
the small number of suitable galaxies in the ESO archive and their
less-than-ideal observing conditions and calibrations. Based on our
experience with these systems, we identify the observational
requirements necessary for the PNLF to yield a competitive value for
H0 that is independent of the Type Ia supernova distance scale.
Description:
For our analysis, we extracted publicly available, fully reduced MUSE
data cubes of 20 galaxies from the ESO archive. These data were
obtained between 2014 June 25 and 2020 December 5; see Table 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 73 1715 MUSE planetary nebulae identifications
table2.dat 57 58 Archival data cubes
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See also:
VII/176 : Photometry and Spectroscopy of Elliptical Galaxies (Faber+ 1989)
VII/180 : Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)
VII/206 : General Photometry of Galaxies (Prugniel+ 1998)
J/ApJ/339/53 : PNe as standard candles. II. (Ciardullo+, 1989)
J/ApJ/356/332 : Planetary nebulae as standard candles. V. (Jacoby+, 1990)
J/ApJ/383/487 : PNe as standard candles. VII. (Ciardullo+, 1991)
J/ApJ/416/62 : Planetary nebulae as standard candles. IX. (McMillan+, 1993)
J/AJ/109/543 : Color of Bright Galaxies (Buta+ 1995)
J/A+A/296/319 : Fornax cluster early-type galaxies (D'Onofrio+, 1995)
J/ApJ/462/1 : PNe in the Coma I region (Jacoby+ 1996)
J/ApJ/479/231 : PNe in M51, M96 & M101 (Feldmeier+ 1997)
J/A+AS/133/325 : Velocities of 12 Fornax elliptical galaxies (Graham+ 1998)
J/AJ/122/2458 : M31 globular clusters from HST (Barmby+, 2001)
J/MNRAS/327/1004 : Early-type galaxy parameters (Blakeslee+, 2001)
J/ApJ/577/31 : PNe in six galaxies (Ciardullo+, 2002)
J/AJ/123/269 : New SMC planetary nebulae (Jacoby+, 2002)
J/A+A/465/71 : 21cm observations of 452 galaxies (Theureau+, 2007)
J/ApJ/703/1569 : Radial distrib. in SINGS galaxies. I. (Munoz-Mateos+, 2009)
J/MNRAS/405/1089 : Photometric scaling for L/S0 galaxies (Laurikainen+ 2010)
J/MNRAS/405/1349 : LMC PNe [OIII]5007Å and Hβ flux (Reid+, 2010)
J/ApJ/730/119 : HST/WFC3 obs. of Cepheids in SN Ia hosts (Riess+, 2011)
J/ApJ/754/67 : Longslit spectroscopy of local bulges (Fabricius+, 2012)
J/MNRAS/444/527 : Tully-Fisher distances for Spitzer galaxies (Sorce+, 2014)
J/ApJ/826/56 : HST/WFC3 obs. of Cepheids in SN Ia host gal. (Riess+, 2016)
J/ApJ/850/207 : Action dynamics of the Local Supercluster (Shaya+, 2017)
J/A+A/611/A58 : SN 2007on and SN 2011iv light curves (Gall+, 2018)
J/ApJS/235/23 : LEGUS galaxies1 observations (Sabbi+, 2018)
J/A+A/611/A95 : Diffuse ionized gas in Antennae galaxy (Weilbacher+, 2018)
J/ApJ/897/122 : Rot. velocities for PHANGS sample of galaxies (Lang+, 2020)
J/A+A/637/A62 : Fornax3D. PNe automated detection (Spriggs+, 2020)
J/A+A/656/A51 : Planetary nebulae in Gaia EDR3 (Gonzalez-Santamaria+, 2021)
J/ApJ/916/21 : OIII PN LFs from MUSE datacubes (Roth+, 2021)
J/A+A/653/A167 : Fornax3D PNe Catalogue (Spriggs+, 2021)
J/A+A/671/A142 : MUSE-PN Catalogue of NGC 300 (Soemitro+, 2023)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Gal Galaxy name
16- 20 A5 --- PNID PN ID sequence number (PNNN within Gal)
23- 26 A4 --- Field Data cube field pointing
29- 37 F9.5 deg RAdeg [11.8/312.2] Right Ascension (J2000)
40- 47 F8.4 deg DEdeg [-47.3/18] Declination (J2000)
49- 54 F6.2 mag m5007 [24.4/31.3] Apparent 5007 magnitude (1)
56- 60 F5.2 mag e_m5007 [0.01/1.3] Uncertainty in 5007 magnitude
62- 69 F8.2 0.1nm lam5007 [5004.28/5061.81] Wavelength of
[OIII]λ5007 emission
73- 73 A1 --- Flag Part of the Statistically Complete Sample? (2)
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Note (1): The total flux of each object was translated into an
[OIII]λ5007 magnitude, m5007 via:
m5007=-2.5logF5007-13.74
where F5007 is the [OIII] line flux in erg/cm2/s. See Section 3.
Note (2): T indicates the PN is part of the sample for used for planetary
nebula luminosity function (PNLF) fitting.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Gal Galaxy name
15- 18 A4 --- Field Field pointing
20- 30 A11 "Y/M/D" Date Observation date (UT)
32- 35 I4 s Exp [621/9600] Exposure time
37- 40 F4.2 arcsec Seeing [0.5/1.8] Archive seeing
42- 52 A11 --- PID ESO program ID; column added by CDS
(see Section 5)
54- 55 I2 --- Fig Figure number in the paper;
column added by CDS (1)
57 A1 --- f_Gal [a] Flag on Gal (2)
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Note (1): For all but two galaxies (NGC 1433 and NGC 2207), we provide an 8s
animation (see the corresponding Figure number in the online paper) that
begins with the off-band image and then steps through the MUSE layers
centered on the galaxy's redshifted [OIII] wavelength. The animation
shows how all emission-line objects, especially the PNe, rise and fall
in brightness with wavelength/velocity (which are noted in the corners
of the video). The animation greatly facilitates the identification of
the PNe compared to the static diff images that are provided.
Note (2): Flag as follows:
a = NGC 1419 information added by CDS from Section 5.9.
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History:
From electronic version of the journal
References:
Roth et al. Paper I. 2021ApJ...916...21R 2021ApJ...916...21R Cat. J/ApJ/916/21
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 07-May-2024