J/A+A/593/A29 Properties of galactic PNe central stars (Moreno-Ibanez+, 2016)
Compact planetary nebulae in the Galactic disk: analysis of the central stars.
Moreno-Ibanez M., Villaver E., Shaw R.A., Stanghellini L.
<Astron. Astrophys. 593, A29 (2016)>
=2016A&A...593A..29M 2016A&A...593A..29M (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; Photometry, HST ; Magnitudes ;
Effective temperatures ; Stars, distances
Keywords: Galaxy: disk - planetary nebulae: general - stars: AGB and post-AGB -
stars: evolution - stars: fundamental parameters
Abstract:
We have obtained multi-wavelength observations of compact Galactic
planetary nebulae (PNe) to probe post-asymptotic giant branch (AGB)
evolution from the onset of nebular ejection. We analyze new
observations from Hubble Space Telescope to derive the masses and
evolutionary status of their central stars (CSs) in order to better
understand the relationship between the CS properties and those of the
surrounding nebulae. We work with HST/WFC3 images of 51 targets
obtained in a snapshot survey (GO-11657). The high spatial resolution
of HST allows us to resolve these compact PNe and distinguish the CS
emission from that of their surrounding PNe. The targets were imaged
through the filters F200LP, F350LP, and F814W from which we derive
Johnson V and I magnitudes. We derive CS bolometric luminosities and
effective temperatures using the Zanstra technique, from a combination
of HST photometry and ground-based spectroscopic data. We present new
unique photometric measurements of 50 CSs, and derived effective
temperatures and luminosities for most of them.
Description:
The photometric information retrieved using HST/WFC3 F200LP, F350LP
and F814W filters allowed us to derive the instrumental magnitudes
using the aperture-corrected methodology. An iterative process which
combines Zanstra methodology and Iraf/STSDAS SYNPHOT tool was
implemented to obtain standard V, I magnitudes and effective
temperatures. Both, Zanstra effective temperatures based on Hβ
and HeII (I(4686)) fluxes are calculated when both fluxes were
available. From the effective temperatures and statistical distances
we obtain the CS luminosities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 99 51 Instrumental and standard V, I magnitudes
tablea2.dat 73 48 *Photometric radii, HI and HeII fluxes,
extinction constants and distances
tablea3.dat 83 47 Zanstra HI and HeII effective temperatures,
luminosities and bolometric correction
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Note on tablea2.dat: All parameters from Stanghellini et al. (2016 ApJ, in press)
except I(4686).
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See also:
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- PNG IAU Commmission 5 name (PN Glll.l+bb.b)
15- 17 A3 --- n_PNG Note on some PNG (1)
19- 23 F5.2 mag F200LP ? Aperture-corrected instrumental magnitude in
filter F200LP (STmag)
28- 31 F4.2 mag e_F200LP ? Uncertainty in F200LP magnitude (STmag)
36- 40 F5.2 mag F350LP ? Aperture-corrected instrumental magnitude in
filter F350LP (STmag)
45- 48 F4.2 mag e_F350LP ? Uncertainty in F350LP magnitude (STmag)
53- 57 F5.2 mag F814W ? Aperture-corrected instrumental magnitude in
filter F814W (STmag)
62- 65 F4.2 mag e_F814W ? Uncertainty in F814W magnitude (STmag)
70- 74 F5.2 mag Vmag ? Standard apparent V magnitude
79- 82 F4.2 mag e_Vmag ? Uncertainty in V magnitude
87- 91 F5.2 mag Imag ? Standard apparent I magnitude
96- 99 F4.2 mag e_Imag ? Uncertainty in I magnitude
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Note (1): Notes as follows:
+ : Central star not detected above the nebular level.
++ : No extinction constant available: transformations to Johnson mags
not possible.
+++ : Central star saturated in all images.
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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- 14 A14 --- PNG IAU Commmission 5 name (PN Glll.l+bb.b)
17- 20 F4.2 --- radPhot Photometric Radius of the central star
21 A1 --- n_radPhot [*] Note on the photometric radius (1)
24- 28 F5.2 mW/m+2 (-logFHb) The log (base 10) of the flux in the
Hβ line of the planetary nebula
31- 34 F4.2 mW/m+2 e_(-logFHb) Uncertainty in the H-β line flux
38- 41 F4.2 --- c Logarithmic extinction constant
45- 48 F4.2 --- E(B-V) Color excess
52 A1 --- l_I(4686) Lower bound for intensity of
HeII 468.6nm line
54- 58 F5.2 --- I(4686) ? Intensity of HeII 468.6nm line on the
usual scale of I(Hβ)=100.
63- 65 A3 --- r_I(4686) ? Original reference of intensity of
HeII 468.6nm line (2)
69- 73 F5.2 kpc Dist Statistical distance
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Note (1): * : photometric radius containing 95% of the flux.
Note (2): References as follows:
1 = Acker et al. (1992secg.book.....A 1992secg.book.....A, Cat. V/84)
2 = Aller & Keyes (1987ApJS...65..405A 1987ApJS...65..405A)
3 = Barker (1978ApJ...219..914B 1978ApJ...219..914B)
4 = Garcia-Hernandez & Gorny (2014A&A...567A..12G 2014A&A...567A..12G)
5 = Kaler & Jacoby (1991ApJ...372..215K 1991ApJ...372..215K)
6 = Lee, Shaw & Stanghellini (2016, in prep.)
7 = Shaw & Kaler (1989ApJS...69..495S 1989ApJS...69..495S)
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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- 14 A14 --- PNG IAU Commmission 5 name (PN Glll.l+bb.b)
18- 23 I6 K Teff(HI) Zanstra effective temperature using
H-β line
26- 30 I5 K e_Teff(HI) Uncertainty in Zanstra Teff(HI)
32 A1 --- l_Teff(HeII) Lower limit flag for Zanstra Teff(HeII)
34- 39 I6 K Teff(HeII) ? Zanstra effective temperature using
HeII 468.6nm line
40 A1 --- n_Teff(HeII) [*] Note on the Zanstra Teff(HeII) (1)
43- 47 I5 K e_Teff(HeII) ? Uncertainty in Zanstra Teff(HeII)
51- 54 F4.2 --- TR ? Ratio of the effective temperatures
55 A1 --- n_TR [+] Note on the temperature ratio (2)
57 A1 --- l_LogL Lower limit flag for luminosity
59- 62 F4.2 [Lsun] LogL Luminosity of the central star compared
to the Sun luminosity
63 A1 --- n_LogL [*] Note on the luminosity (1)
67- 70 F4.2 [Lsun] e_LogL ? Uncertainty in the luminosities
72 A1 --- l_BC Upper limit flag for bolometric correction
74- 78 F5.2 mag BC Bolometric correction
80- 83 F4.2 mag e_BC ? Uncertainty in bolometric correction
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Note (1): *: I(4686)>90 suggests nebula is optically thin in He+, so T(HeII)
and L(HeII) are lower limits.
Note (2): +: May be optically thick in H Lyman based on surface brightness.
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Acknowledgements:
Manuel Moreno-Ibanez, mmoreno(at)ice.csic.es
(End) M. Moreno-Ibanez [ICE(IEEC-CSIC), Spain], P. Vannier [CDS] 11-Jul-2016