J/AJ/156/300 Velocity and light curve analysis of three PPNe (Hrivnak+, 2018)
Variability in proto-planetary nebulae.
V. Velocity and light curve analysis of IRAS 17436+5003, 18095+2704,
and 19475+3119.
Hrivnak B.J., Van de Steene G., Van Winckel H., Lu W., Sperauskas J.
<Astron. J., 156, 300 (2018)>
=2018AJ....156..300H 2018AJ....156..300H (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; Stars, giant ; Photometry, UBVRI ;
Radial velocities ; Spectral types ; Effective temperatures ;
Abundances
Keywords: stars: AGB and post-AGB -
stars: individual (IRAS 17436+5003, IRAS 18095+2704,
IRAS 19475+3119) - stars: oscillations (including pulsations) -
stars: variables: general
Abstract:
We have obtained contemporaneous light, color, and radial velocity data
for three proto-planetary nebulae (PPNe) over the years 2007 to 2015.
The light and velocity curves of each show similar periods of pulsation,
with photometric periods of 42 and 50 days for IRAS 17436+5003, 102 days
for IRAS 18095+2704, and 35 days for IRAS 19475+3119. The light and
velocity curves are complex with multiple periods and small, variable
amplitudes. Nevertheless, at least over limited time intervals, we were
able to identify dominant periods in the light, color, and velocity curves
and compare the phasing of each. The color curves appear to peak with
or slightly after the light curves while the radial velocity curves peak
about a quarter of a cycle before the light curves. Similar results were
found previously for two other PPNe, although for them the light and
color appeared to be in phase. Thus, it appears that PPNe are brightest
when smallest and hottest. These phase results differ from those found
for classical Cepheid variables, where the light and velocity differ
by half a cycle, and are hottest at about average size and expanding.
However, they do appear to have similar phasing to the larger-amplitude
pulsations seen in RV Tauri variables. Presently, few pulsation models
exist for PPNe, and these do not fit the observations well, especially
the longer periods observed. Model fits to these new light and velocity
curves would allow masses to be determined for these post-AGB objects,
and thereby provide important constraints to post-AGB stellar evolution
models of low- and intermediate-mass stars.
Description:
We have carried out radial velocity observations of these three objects
using high-resolution spectra observed with four different
telescope-spectrograph-detector systems. The initial observations were
carried out at the Dominion Astrophysical Observatory (DAO) in Victoria,
Canada, using the Radial Velocity Spectrometer at the Coude focus of
the 1.2 m telescope. This used a physical mask based on an F star and
covered the spectral range 4000-4600 Å. Most of the data are from
1991 to 1993. We will refer to these as the DAO-RVS observations. We
re-initiated the radial velocity program at the DAO in 2007, using a
CCD (DAO-CCD) and covering a smaller spectral region, 4350-4500 Å.
The study was expanded to include radial velocities observations for all
three objects with the the Flemish 1.2 m Mercator Telescope on La Palma
and additional observations of IRAS 17436+5003 with the 1.65 m telescope
of the Moletai Observatory (Lithuania). The Mercator observations began
in 2009 and used the HERMES fiber-fed echelle spectrograph (Raskin et al.
2011A&A...526A..69R 2011A&A...526A..69R) and covered the spectral range 4770-6550 Å. The
Moletai Observatory spectra covered the interval 3850-6400 Å and used
a physical CORAVEL mask based primarily on the solar spectrum. These
Moletai observations were carried out from 2008 to 2014.
New photometric observations of these objects were carried out from 2013
to 2015 at the Valparaiso University Observatory (VUO). These were obtained
with an 0.4 m telescope equipped with an SBIG 6303 CCD camera and
standardized to the Johnson B and V and Cousins RC systems. Differential
photometry was employed, using an aperture of 11" diameter, as was used
in our previous studies. An observation consists of a single exposure
in a filter per night. Note that we do not have B data from 2015. Typical
exposure times ranged from 6 s for IRAS 17436+5003 to 2 minutes for
IRAS 18095+2704.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 73 6 Program objects
table3.dat 25 392 Radial velocities for IRAS 17436+5003
table4.dat 25 200 Radial velocities for IRAS 18095+2704
table5.dat 25 172 Radial velocities for IRAS 19475+3119
table6.dat 31 161 Differential standard BVRC magnitudes for
IRAS 17436+5003 from 2013-2015
table7.dat 31 120 Differential standard BVRC magnitudes for
IRAS 18095+2704 from 2013-2015
table8.dat 31 124 Differential standard BVRC magnitudes for
IRAS 19475+3119 from 2013-2015
table9.dat 78 32 Periodogram study of the radial velocity curves
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See also:
J/A+AS/126/479 : NIR photometry of IRAS sources. III (Garcia-Lario+, 1997)
J/ApJS/122/221 : A mid-IR survey of Proto-PNs Candidates (Meixner+, 1999)
J/A+A/368/250 : Abundances of HDE 341617 (Arellano Ferro+, 2001)
J/A+A/458/173 : Optical spectroscopy of 253 IRAS sources (Suarez+, 2006)
J/PASJ/59/1127 : Abundances in 5 post-AGB candidates (Takeda+, 2007)
J/ApJ/709/1042 : Variability in C-rich proto-PNe. (Hrivnak+, 2010)
J/PAZh/36/281 : Variability of 3 protoplanetary nebulae (Arkhipova+, 2010)
J/ApJ/766/116 : Variability in proto-PNe. II. (Hrivnak+, 2013)
J/AJ/149/184 : Long-term photometry for 4 O-rich PPne (Hrivnak+, 2015)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- IRAS IRAS identifier
12- 15 F4.1 mag Vmag [7/10]? V band magnitude (1)
17- 19 F3.1 mag B-V [0.6/1]? B-V color index (2)
21- 23 F3.1 mag V-Rc [0.2/0.7]? V-RC color index
25- 29 A5 --- SpType Spectral type
31- 34 I4 K Teff [6500/7750] Effective temperature
36- 38 F3.1 [cm/s2] logg [0/1.1] Surface gravity
40- 43 F4.1 [-] [Fe/H] [-0.9/-0.2] Abundance ratio [Fe/H]
45- 48 F4.1 [-] [C/O] [-0.5/-0.2] Abundance ratio [C/O]
50 I1 --- Ref [1/5] Reference for the spectroscopic analyse
(3)
52 A1 --- n_IRAS [d] Note on IRAS (4)
54- 73 A20 --- OtherID Other identifiers
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Note (1): Variable.
Note (2): Variable. Includes circumstellar and interstellar reddening.
Note (3): Reference as follows:
1 = Luck et al. (1990ApJ...357..188L 1990ApJ...357..188L);
2 = Klochkova et al. (2002AstL...28...49K 2002AstL...28...49K);
3 = Takeda et al. (2007, J/PASJ/59/1127);
4 = Sahin et al. (2011, J/A+A/458/173);
5 = Arellano Ferro et al. (2001, J/A+A/368/250).
Note (4): Note as follows:
d = Several He lines measured, suggesting He overabundance (Klochkova et al.
2002AstL...28...49K 2002AstL...28...49K).
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Byte-by-byte Description of file: table3.dat table4.dat table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.4 d HJD [48431.8452/57510.7276] Heliocentric Julian Date
(HJD-2400000)
12- 17 F6.2 km/s RV [-60.7/9] Radial velocity (1)
19- 25 A7 --- SpecID Spectrograph-detector system
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Note (1): These are the radial velocities as measured on the individual
spectrograph-detector systems, without the inclusion of the
empirically-determined offsets. See the text for details and offset values.
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Byte-by-byte Description of file: table6.dat table7.dat table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.4 d HJD [56436.6855/57358.5088] Heliocentric Julian Date
(HJD-2400000) (1)
12- 17 F6.3 mag DBmag [-3.942/-1.063]? Differential Johnson B magnitude
(2)
19- 24 F6.3 mag DVmag [-3.441/-1.62]? Differential Johnson V magnitude
(2)
26- 31 F6.3 mag DRcmag [-3.203/-1.944]? Differential Cousins RC
magnitude (2)
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Note (1): The time represents the mid-time of the V observation. The times for
the B and RC observations differ from this by approximately the following:
+0.0011 and -0.0012 days, respectively.
Note (2): The average uncertainties in the differential magnitudes are ±0.005.
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Byte-by-byte Description of file: table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- IRAS IRAS identifier
12- 22 A11 --- Set Data set
24- 27 I4 yr Year1 [1978/2015] First year of observation
29- 32 I4 yr Year2 [1979/2015]? Last year of observation
34- 36 I3 --- Nobs [11/333] Number of observations
38- 43 F6.2 km/s A0 [-53.96/2.28] Systemic velocity (1)
44 A1 --- n_A0 [d] Note on A0 (2)
46- 51 F6.2 d Per1 [35.04/109.2]? Primary period
52 A1 --- u_Per1 [:)] Uncertainty flag on Per1 (3)
53 A1 --- n_Per1 [e] Note on Per1 (4)
55- 58 F4.2 km/s A1 [1.08/5.1]? Primary amplitude
60- 63 F4.2 --- phi1 [0.09/0.99]? Primary phase φ1 (5)
65- 68 F4.1 d Per2 [33.3/46.6]? Secondary period
70- 73 F4.2 km/s A2 [1.43/2.3]? Secondary amplitude
75- 78 F4.2 --- phi2 [0.13/0.92]? Secondary phase φ2 (5)
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Note (1): The systemic velocities listed in the table for the individual data
sets are as observed, without an offset. For combined data sets, offsets are
added to the DAO and CORAVEL data sets to bring them to the HERMES system.
Note (2): Note as follows:
d = The average velocity is listed in the absence of a systemic velocity
determined from a period analysis.
Note (3): Uncertainty flag as follows:
: = Period values that are not quite significant;
) = Period values that are more uncertain.
Note (4): Note as follows:
e = Period fixed at the value determined from the V light curve during the
associated years.
Note (5): The phases are determined based on the epoch of JD 2455600.00.
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History:
From electronic version of the journal
References:
Hrivnak et al. Paper I. 2010ApJ...709.1042H 2010ApJ...709.1042H Cat. J/ApJ/709/1042
Hrivnak et al. Paper II. 2013ApJ...766..116H 2013ApJ...766..116H Cat. J/ApJ/766/116
Hrivnak et al. Paper III. 2015ApJ...805...78H 2015ApJ...805...78H
Hrivnak et al. Paper IV. 2015AJ....149..184H 2015AJ....149..184H Cat. J/AJ/149/184
Hrivnak et al. Paper V. 2018AJ....156..300H 2018AJ....156..300H This catalog
Hrivnak et al. Paper VI. 2020AJ....159...21H 2020AJ....159...21H Cat. J/AJ/159/21
Hrivnak et al. Paper VII. 2020ApJ...901....9H 2020ApJ...901....9H Cat. J/ApJ/901/9
Hrivnak et al. Paper VIII. 2021AJ....162..248H 2021AJ....162..248H
Hrivnak et al. Paper IX. 2022ApJ...939...32H 2022ApJ...939...32H Cat. J/ApJ/939/32
Hrivnak et al. Paper X. 2024AJ....167...30H 2024AJ....167...30H Cat. J/AJ/167/30
(End) Prepared by [AAS] Tiphaine Pouvreau [CDS] 30-Apr-2019