J/A+A/686/A72 MUSE datacubes of T Pyx (Izzo+, 2024)
The physical properties of T Pyx as measured by MUSE.
I. The geometrical distribution of the ejecta and the distance to the remnant.
Izzo L., Pasquini L., Aydi E., Della Valle M., Gilmozzi R., Harvey E.A.,
Molaro P., Otulakowska-Hypka M., Selvelli P., Thoene C.C., Williams R.
<Astron. Astrophys. 686, A72 (2024)>
=2024A&A...686A..72I 2024A&A...686A..72I (SIMBAD/NED BibCode)
ADC_Keywords: Supernova remnants ; Infrared ; Photometry, H-alpha
Keywords: stars: distances - novae - cataclysmic variables - white dwarfs
Abstract:
T Pyx is one of the most enigmatic recurrent novae, and it has been
proposed as a potential Galactic type-Ia supernova
progenitor.
Using spatially resolved data obtained with MUSE, we characterized the
geometrical distribution of the material expelled in previous
outbursts surrounding the white dwarf progenitor
We used a 3D model for the ejecta to determine the geometric
distribution of the extended remnant. We also calculated the nebular
parallax distance (d=3.55±0.77kpc) based on the measured
velocity and spatial shift of the 2011 bipolar ejecta. Our findings
confirm previous results, including the data from the GAIA mission.
The remnant of T Pyx can be described by a two-component model
consisting of a tilted ring at i=63.7 relative to its normal vector
and fast bipolar ejecta perpendicular to the plane of the equatorial
ring.
We found an upper limit for the bipolar outflow ejected mass in 2011
of the bipolar outflow of Mej,b<(3.0±1.0)x10-6M☉, which is
lower than previous estimates given in the literature. However, only a
detailed physical study of the equatorial component can provide an
accurate estimate of the total ejecta of the last outburst, a
fundamental step to understanding if T Pyx will end its life as a
type-Ia supernova.
Description:
The remnant of the RN T Pyx has been observed with MUSE, which is
mounted on the UT4 (Yepun) at the European Southern Observatory Very
Large Telescope located in Paranal, Chile.
The NFM observations were done on November 15, 2021.
The WFM observations were performed on January 1 and 9, 2022.
Objects:
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RA (2000) DE Designation(s)
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09 04 41.50 -32 22 47.5 T Pyx = TIC 17897279
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 145 2 List of fits datacubes
fits/* . 2 Individual fits datacubes
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See also:
J/A+A/310/173 : TY Pyx IUE FES observations (Neff+, 1996)
J/A+A/622/A126 : T Pyx 2011 outburst optical spectra (Pavana+, 2019)
J/other/BASI/39.259 : WX Pyx J-band light curve (Joshi+, 2011)
J/ApJ/773/55 : Light curve of T Pyx from 1890 to 2011 (Schaefer+, 2013)
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 25 F6.4 arcsec/pix scale Scale of the image
27- 29 I3 --- Nx Number of pixels along X-axis
31- 33 I3 --- Ny Number of pixels along Y-axis
35- 38 I4 --- Nz Number of slices
40- 62 A23 "datime" Obs.date Observation date
64- 70 F7.2 0.1nm bAWAV Lower value of wavelength interval
72- 78 F7.2 0.1nm BAWAV Upper value of wavelength interval
80- 83 F4.2 0.1nm dAWAV Wavelenght resolution
85- 91 I7 Kibyte size Size of FITS file
93-121 A29 --- FileName Name of FITS file, in subdirectory fits
123-145 A23 --- Title Title of the FITS file
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Acknowledgements:
Luca Izzo, luca.izzo(at)inaf.it
(End) Patricia Vannier [CDS] 07-May-2024