J/A+A/659/A145 A WISE view on extreme AGB stars (Groenewegen, 2022)
A WISE view on extreme AGB stars.
Groenewegen M.A.T.
<Astron. Astrophys. 659, A145 (2022)>
=2022A&A...659A.145G 2022A&A...659A.145G (SIMBAD/NED BibCode)
ADC_Keywords: Infrared sources ; Magellanic Clouds ; Stars, late-type ;
Stars, variable ; Stars, distances
Keywords: stars: variables: general - infrared: stars -
stars: AGB and post-AGB
Abstract:
Variability is a key property of stars on the asymptotic giant branch
(AGB). Their pulsation period is related to the luminosity and
mass-loss rate (MLR) of the star. Long-period variables (LPVs) and
Mira variables are the most prominent of all types of variability of
evolved stars. However, the reddest, most obscured AGB stars are too
faint in the optical and have eluded large variability surveys.
Our goal is to obtain a sample of LPVs with large MLRs by analysing
WISE W1 and W2 light curves (LCs) for about 2000 sources,
photometrically selected to include known C-stars with the 11.3 micron
silicon carbide dust feature in absorption, and Galactic O-stars with
periods longer than 1000 days.
Epoch photometry was retrieved from the AllWISE and NEOWISE database
and fitted with a sinus curve. Photometry from other variability
surveys was also downloaded and fitted.
For a subset of 316 of the reddest stars, spectral energy
distributions (SEDs) were constructed, and, together with mid-infrared
(MIR) spectra when available, fitted with a dust radiative transfer
programme in order to derive MLRs.
WISE based LCs and fits to the data are presented for all stars.
Periods from the literature and periods from refitting other
literature data are presented. The results of the spatial correlation
with several (IR) databases is presented. About one-third of the
sources are found to be not real, but it appears that these cannot be
easily filtered out by using WISE flags. Some are clones of extremely
bright sources, and in some cases the LCs show the known pulsation
period.
Inspired by a recent paper, a number of non-variable OH/IRs are
identified. Based on a selection on amplitude, a sample of about 750
(candidate) LPVs is selected of which 145 have periods beyond 1000
days, many of them being new.
For the subset of the stars with the colours of C-rich extremely red
objects (EROs) the fitting of the SEDs (and available MIR spectra)
separates them into C- and O-rich objects.
Interestingly, the fitting of MIR spectra of mass-losing C-stars is
shown to be a powerful tracer of interstellar reddening when AV larger
than 2 mag.
The number of Galactic EROs appears to be complete up to about 5 kpc
and a total dust return rate in the solar neighbourhood for this class
is determined.
In the LMC 12 additional EROs are identified. Although this represents
only about 0.15% of the total known LMC C-star population adding their
MLRs increases the previously estimated dust return by 8%.
Based on the EROs in the Magellanic Clouds, a bolometric period
luminosity is derived.
It is pointed out that due to their faintness, EROs and similar O-rich
objects are ideal targets for a NIR version of Gaia to obtain
distances, observing in the K-band or, even more efficiently, in the
L-band.
Description:
The tabular material describes
1) the properties and the derived light-curve parameters for the
sample of 1992 stars, which are divided into 1224 sources with periods
derived from WISE data, 118 sources with periods derived from the
literature or refitting timeseries data other than WISE, and 650
sources that are likely not real, and
2) the results of the fitting of the SEDs of 316 of the reddest
sources that are divided into 197 likely C-stars and 119 likely O-rich
objects.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 102 197 Fit results of C-stars
tablea1.dat 160 1223 Bona fide stellar sources with a period analysis
based on WISE data, general information
tablea2.dat 271 1223 Bona fide stellar sources with a period analysis
based on WISE data, period analysis based
on WISE data
tablea3.dat 155 118 Bona fide stellar sources with a period analysis
based on literature data, general information
tablea4.dat 141 118 Bona fide stellar sources with a period analysis
based on literature data, period analysis based
on WISE data
tablea5.dat 165 651 Likely non bona fide sources,
general information
tablea6.dat 178 651 Likely non bona fide sources,
period analysis based on WISE data
tablec1.dat 102 119 Fit results of O-rich objects
refs.dat 204 38 References
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Byte-by-byte Description of file: table2.dat tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.6 deg RAdeg Right Ascension (J2000)
12- 21 F10.6 deg DEdeg Declination (J2000)
23- 26 I4 d Per Period used in the PL-relation
28- 32 F5.2 kpc Dist Distance
34- 38 F5.2 mag Av Interstellar extinction in the V-band
40- 44 I5 K Teff Effective temperature
46- 52 I7 Lsun L Luminosity
54- 59 I6 Lsun e_L Luminosity error
61- 64 I4 --- tau Dust optical depth at 0.5 micron
66- 70 F5.1 --- e_tau Dust optical depth at 0.5 micron
72- 76 I5 K Tc Condensation temperature
78- 80 I3 K e_Tc Condensation temperature error
82 I1 --- fTc [0/1] Was the condensation temperature
fitted (1) or fixed (0)
84- 86 F3.1 --- p Slope of the density law
88- 90 F3.1 --- e_p Slope of the density law error
92 I1 --- fp [0/1] Was the slope fitted (1) or fixed (0)
94-102 E9.4 Msun/yr Mdot Gas mass-loss rate
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat tablea3.dat tablea5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.6 deg RAdeg Right Ascension (J2000)
12- 21 F10.6 deg DEdeg Declination (J2000)
23- 66 A44 --- Ident Identifiers
68- 71 F4.2 arcsec Dist ? Distance to nearest SIMBAD object
73- 83 A11 --- ObjT Object type in SIMBAD
85- 87 F3.1 arcsec 2M ? Distance to the closest 2MASS source
within 1", if any
89- 91 F3.1 arcsec GLP ? Distance to the closest GLIPMSE source
within 3", if any
93- 95 F3.1 arcsec Aka ? Distance to the closest Akari/IRC source
within 3", if any
97- 99 F3.1 arcsec MSX ? Distance to the closest MSX source
within 5", if any
101-103 F3.1 arcsec MGL ? Distance to the closest MIPSGAL source
within 2", if any
105-107 F3.1 arcsec HGL ? Distance to the closest Herschel Hi-GAL
source within 4.5", if any
109-114 F6.1 km/s Vb ?=- Blue velocity of a OH maser source, if any
115 A1 --- n_Vb [n] n for observed but not detected
116-121 F6.1 km/s Vr ?=- Red velocity of a OH maser source, if any
122 A1 --- n_Vr [n] n for observed but not detected
123 A1 --- LRS IRAS LRS type from Kwok et al.,
1997ApJS..112..557K 1997ApJS..112..557K, Cat. J/ApJS/112/557
125-150 A26 --- SpType Spectral types from Skiff, 2014, Cat. B/mk
152-165 A14 --- Refs References for extragalactic catalogues (1)
--------------------------------------------------------------------------------
Note (1): References for extragalactic catalogues:
Q = probable QSOs
q = candidate QSOs
(1) = Flesch, 2015PASA...32...10F 2015PASA...32...10F, Cat. VII/290
(2) = Bailer-jones et al., 2019MNRAS.490.5615B 2019MNRAS.490.5615B, Cat. VII/285
(3) = Guo et al., 2018A&A...618A.144G 2018A&A...618A.144G, Cat. J/A+A/618/A144
(4) = Assef et al., 2018ApJS..234...23A 2018ApJS..234...23A, Cat. J/ApJS/234/23
(5) = Gaia Collaboration et al., 2021A&A...649A...9G 2021A&A...649A...9G
(6) = Solarz et al., 2017A&A...606A..39S 2017A&A...606A..39S, Cat. J/A+A/606/A39
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Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.6 deg RAdeg Right Ascension (J2000)
12- 21 F10.6 deg DEdeg Declination (J2000)
23- 27 I5 d Plit1 ? Period from first reference
28 A1 --- u_Plit1 Uncertainty flag on Plit1
29 A1 --- --- [|/]
30- 33 I4 d Plit1u ? Second Period from first reference
35- 37 I3 d e_Plit1 ? rms uncertainty on Plit1
39- 40 A2 --- n_Plit1 [no ] n for no
41 A1 --- --- [(]
42- 43 I2 --- r_Plit1 ? Reference for Plit1
44 A1 --- --- [)]
45 A1 --- --- [,]
46- 51 F6.1 d Plit2 ? Period from second reference
52 A1 --- uPlit2 Uncertainty flag on Plit2
53 A1 --- --- [/]
54- 56 I3 d Plit2u ? Second Period from second reference
57 A1 --- --- [|]
58- 62 F5.1 d e_Plit2u ? rms uncertainty on Plit2
63 A1 --- ue_Plit2u Uncertainty flag on e_Plit2u
65- 66 A2 --- n_Plit2 [no ]
67 A1 --- --- [(]
68- 69 I2 --- r_Plit2 ? Reference for Plit2
70 A1 --- --- [)]
71 A1 --- --- [,]
72- 75 I4 d Plit3 ? Period from third reference
76 A1 --- u_Plit3 Uncertainty flag on Plit3
77 A1 --- --- [/]
78- 81 I4 d Plit3u ? Second Period from third reference
82 A1 --- --- [|]
83- 85 I3 d e_Plit3 ? rms uncertainty on Plit3
87- 88 A2 --- n_Plit3 [no ]
89 A1 --- --- [(]
90- 91 I2 --- r_Plit3 ? Reference for Plit3
92 A1 --- --- [)]
93 A1 --- --- [,]
94- 97 I4 d Plit4 ? Period from reference 4
98 A1 --- --- [|]
99-101 I3 d e_Plit4 ? rms uncertainty on Plit4
102-103 A2 --- n_Plit4 [no ]
104 A1 --- --- [(]
105-106 I2 --- r_Plit4 ? Reference for Plit4
107 A1 --- --- [)]
108 A1 --- --- [,]
110-112 I3 d Plit5 ? Period from reference 6
113 A1 --- --- [|]
114-115 I2 d e_Plit5 ? rms uncertainty on Plit5
117 A1 --- --- [(]
118-119 I2 --- r_Plit5 ? Reference for Plit5
120 A1 --- --- [)]
122-127 F6.1 d Prefit1 ? Period from refitting non-WISE data,
first reference
128 A1 --- u_Prefit1 Uncertainty flag on Prefit1
129 A1 --- --- [|]
130-132 I3 d e_Prefit1 ? rms uncertainty on Prefit1
134 A1 --- --- [(]
135-136 I2 ---- r_Prefit1 ? Reference for Prefit1
137 A1 --- --- [)]
138 A1 --- --- [,]
139-142 I4 d Prefit2 ? Period from refitting non-WISE data,
second reference
143 A1 --- --- [|]
144-147 F4.1 d e_Prefit2 ? rms uncertainty on Prefit2
149 A1 --- --- [(]
150-151 I2 --- r_Prefit2 ? Reference for Prefit2
152 A1 --- --- [)]
153 A1 --- --- [,]
155-156 I2 d Prefit3 ? Period from refitting non-WISE data,
third reference
158 A1 --- --- [(]
159-160 I2 --- r_Prefit3 ? Reference for Prefit3
161 A1 --- --- [)]
163-167 I5 d P1 ? Period from fitting W1 data
169-174 F6.1 d e_P1 ? Error on P1
176-180 I5 d P2 ? Period from fitting W2 data
182-188 F7.1 d e_P2 ? Error on P2
190-193 F4.2 mag Amp1 Fitted amplitude in the W1 filter
195-200 F6.2 mag e_Amp1 Error on Amp1
206-211 F6.3 mag W1 Mean W1 magnitude
213-218 F6.3 mag e_W1 Error on W1
220-225 F6.1 --- chirW1 Reduced chi2 of the fit in the W1 filter
227-230 F4.2 mag Amp2 Fitted amplitude in the W2 filter
233-238 F6.2 mag e_Amp2 Error on Amp2
240-245 F6.3 mag W2 Mean W2 magnitude
247-252 F6.3 mag e_W2 Error on W2
254-259 F6.1 --- chirW2 Reduced chi2 of the fit in the W2 filter
261-262 I2 --- Com ? Comment (G2)
264-271 A8 --- Class Class (G3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.6 deg RAdeg Right Ascension (J2000)
12- 21 F10.6 deg DEdeg Declination (J2000)
23- 26 I4 d Plit1 ? Period from first reference
27 A1 --- u_Plit1 Uncertainty flag on Plit1
28 A1 --- --- [|/]
29- 31 I3 d Plit1u ? Second Period from first reference
32 A1 --- --- [|]
33- 35 I3 d e_Plit1 ? rms uncertainty on Plit1
37- 38 A2 --- n_Plit1 [no ]
39 A1 --- --- [(]
40- 41 I2 --- r_Plit1 ? Reference for Plit1 (G1)
42 A1 --- --- [)]
43 A1 --- --- [,]
44- 47 I4 d Plit2 ? Period from second reference
48 A1 --- --- [/]
49- 51 I3 d Plit2u ? Second Period from second reference
52 A1 --- --- [|]
53- 54 I2 d e_Plit2u ? rms uncertainty on Plit2
56- 57 A2 --- n_Plit2 [no ]
58 A1 --- --- [(]
59- 60 I2 --- r_Plit2 ? Reference for Plit2 (G1)
61 A1 --- --- [)]
62 A1 --- --- [,]
63- 66 I4 d Plit3 ? Period from third reference
67 A1 --- --- [|]
68- 69 I2 d e_Plit3 ? rms uncertainty on Plit3
70- 71 A2 --- n_Plit3 [no ]
72 A1 --- --- [(]
73- 74 I2 --- r_Plit3 ? Reference for Plit3 (G1)
75 A1 --- --- [)]
76 A1 --- --- [,]
77- 80 I4 d Plit4 ? Period from reference 4
81 A1 --- u_Plit4 [)] Uncertainty flag on Plit4
82- 84 I3 d e_Plit4 ? rms uncertainty on Plit4
86 A1 --- --- [(]
87- 88 I2 --- r_Plit4 ? Reference for Plit4 (G1)
89 A1 --- --- [)]
90 A1 --- --- [,]
91- 94 I4 d Plit5 ? Period from reference 5
96 A1 --- --- [(]
97- 98 I2 --- r_Plit5 ? Reference for Plit5 (G1)
99 A1 --- --- [)]
101-103 I3 d Prefit1 ? Period from refitting non-WISE data,
first reference
104 A1 --- --- [|]
105-106 I2 d e_Prefit1 ? rms uncertainty on Prefit1
108 A1 --- --- [(]
109-110 I2 --- r_Prefit1 ? Reference for Prefit2 (G1)
111 A1 --- --- [)]
112 A1 --- --- [,]
113-115 I3 d Prefit2 ? Period from refitting non-WISE data,
second reference
116 A1 --- --- [|]
117 I1 d e_Prefit2 ? rms uncertainty on Prefit2
119 A1 --- --- [(]
120-121 I2 --- r_Prefit2 ? Reference for Prefit2 (G1)
122 A1 --- --- [)]
123 A1 --- --- [,]
124-126 I3 d Prefit3 ? Period from refitting non-WISE data,
third reference
127 A1 --- --- [|]
128 A1 d e_Prefit3 ? rms uncertainty on Prefit3
130 A1 --- --- [(]
131-132 I2 --- r_Prefit3 ? Reference for Prefit3 (G1)
133 A1 --- --- [)]
135-136 I2 --- Com ? Comment (G2)
138-141 A4 --- Class Class (G3)
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Byte-by-byte Description of file: tablea6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.6 deg RAdeg Right Ascension (J2000)
12- 21 F10.6 deg DEdeg Declination (J2000)
23- 25 I3 d Plit1 ? Period from first reference
27 A1 --- --- [(]
28- 29 I2 --- r_Plit1 ? rms uncertainty on Plit1
30 A1 --- --- [)]
31 A1 --- --- [,]
32- 33 I2 d Plit2 ? Period from second reference
35 A1 --- --- [(]
36- 37 I2 --- r_Plit2 ? rms uncertainty on Plit2
38 A1 --- --- [)]
40- 43 I4 d P1 ? Period from fitting W1 data
45- 50 F6.1 d e_P1 ? Error on P1
58- 61 I4 d P2 ? Period from fitting W2 data
63- 68 F6.1 d e_P2 ? Error on P2
76- 79 F4.2 mag Amp1 ? Fitted amplitude in the W1 filter
82- 85 F4.2 mag e_Amp1 ? Error on Amp1
94- 99 F6.3 mag W1 ? Mean W1 magnitude
101-105 F5.3 mag e_W1 ? Error on W1
113-119 F7.1 --- chirW1 ? Reduced chi2 of the fit in the W1 filter
128-131 F4.2 mag Amp2 ? Fitted amplitude in the W2 filter
134-137 F4.2 mag e_Amp2 ? Error on Amp2
146-151 F6.3 mag W2 ? Mean W2 magnitude
153-157 F5.3 mag e_W2 ? Error on W2
165-170 F6.1 --- chirW2 ? Reduced chi2 of the fit in the W2 filter
172-173 I2 --- Com ? Comment (G2)
175-178 A4 --- Class Class (G3)
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 46 A23 --- Aut Authors' name
47-204 A158 --- Com Comments
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Global notes:
Note (G1): References in ref.dat file
Note (G2): Comments as follows:
1 = W2 data is dummy
2 = Possibly a real source. IRAS 02408+5458 is located at 3arcsec
3 = ASAS-SN: LC is peculiar
4 = Palt = 572 days
5 = ZTF: LC is peculiar
6 = Clones of VY CMa (110.7430362 -25.7675659)
7 = Source is getting fainter with time
8 = Clones of IRAS 08074-3615 (122.334335 -36.407444)
9 = Clones of HD 76220 (133.849921103 +19.6998172)?
10 = Palt = 262 days
11 = Peculiar LC
12 = Palt = 491 days
13 = Source is getting brighter with time
14 = A clone of CW Leo (146.989203 +13.278759)
15 = Source is getting brighter with time
16 = Clones of HD 97300 (167.4575881 -76.6130701)
17 = Possibly a clone of IRAS 11145-6534, located at 75arcsec
18 = ASAS-SN: bizarre LC
19 = Possibly a real source. Not an obvious clone
20 = A clone of IRAS 15194-5115 (230.7711108 -51.4329088)
21 = Source (W2) is getting fainter with time
22 = Source (W2) is getting fainter with time
23 = Palt = 580, 780 days
24 = Palt = 1280 days
25 = Palt = 800 days
26 = Source is getting fainter with time
27 = Palt = 303 days
28 = Palt = 460 days
29 = P = 34.48±0.16 days
30 = Palt = 460 days
31 = A clone of IRC +20 326 (262.9805754 +17.7558379)
32 = Palt = 480, 730 days
33 = W1 data is dummy
34 = Palt = 314 days
35 = Palt = 969 days
36 = Sakurais object. Continueously brightening in K (VVV) and WISE filters
37 = Palt = 460, 301 days
38 = Palt = 355 days
39 = A clone of AFGL 2135 (275.644226 -27.108224)
40 = ASAS-SN: Burst, then nearly constant
41 = Source is getting fainter with time
42 = ZTF: peculiar LC (period fixed to 600 days)
43 = ATLAS: Slowly getting brighter, with burst (?)
44 = ZTF: very peculiar LC
45 = Palt = 1900 days
46 = ATLAS, ZTF: peculiar LC. Strong drop in brightness
47 = Source (W1) is getting brighter with time
48 = Palt = 330 days
49 = Clones of IRC +10 420 (291.700408 +11.354634)
50 = OMC, ZTF: Slow change in both datasets
51 = ZTF: very peculiar LC
52 = P = 30.58±0.02 days
53 = ASAS-SN: constant but then strong brightening
54 = ZTF: very peculiar LC
55 = Clones of AFGL 3068 (349.802533 +17.192628)
56 = A clone of AFGL 3116 (353.61467 +43.55036)
Note (G3): Class as follows:
LPV = LPVs as defined by the criteria in Sect. 6.4
PER = Interesting non-LPV sources, some of which may be periodic
NVOH = Known non-variable OH/IR stars from the literature
nvoh = Candidate non-variable OH/IR stars from this work
ERO = Template EROs from Table 1
eroP = Candidate EROs based on photometry
eroS = Candidate EROs based on photometry and MIR spectra
sedC = Non-ERO stars classified as C-rich based on SED fitting
sedO = Stars classified as O-rich based on SED fitting
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Acknowledgements:
Martin Groenewegen, martin.groenewegen(at)oma.be
(End) Patricia Vannier [CDS] 26-Jan-2022