J/ApJS/257/49 Five decades 1-40GHz obs. of 36 classical novae (Chomiuk+, 2021)
Classical novae at radio wavelengths.
Chomiuk L., Linford J.D., Aydi E., Bannister K.W., Krauss M.I.,
Mioduszewski A.J., Mukai K., Nelson T.J., Rupen M.P., Ryder S.D.,
Sokoloski J.L., Sokolovsky K.V., Strader J., Filipovic M.D., Finzell T.,
Kawash A., Kool E.C., Metzger B.D., Nyamai M.M., Ribeiro V.A.R.M., Roy N.,
Urquhart R., Weston J.
<Astrophys. J. Suppl. Ser., 257, 49 (2021)>
=2021ApJS..257...49C 2021ApJS..257...49C
ADC_Keywords: Novae; Radio sources ; References
Keywords: Cataclysmic variable stars ; Novae ; Radio transient sources ;
White dwarf stars ; Galactic radio sources
Abstract:
We present radio observations (1-40GHz) for 36 classical novae,
representing data from over five decades compiled from the literature,
telescope archives, and our own programs. Our targets display a
striking diversity in their optical parameters (e.g., spanning optical
fading timescales, t2=1-263days), and we find a similar diversity in
the radio light curves. Using a brightness temperature analysis, we
find that radio emission from novae is a mixture of thermal and
synchrotron emission, with nonthermal emission observed at earlier
times. We identify high brightness temperature emission
(TB>5x104K) as an indication of synchrotron emission in at least
nine (25%) of the novae. We find a class of synchrotron-dominated
novae with mildly evolved companions, exemplified by V5589 Sgr and
V392 Per, that appear to be a bridge between classical novae with
dwarf companions and symbiotic binaries with giant companions. Four of
the novae in our sample have two distinct radio maxima (the first
dominated by synchrotron and the later by thermal emission), and in
four cases the early synchrotron peak is temporally coincident with a
dramatic dip in the optical light curve, hinting at a common site for
particle acceleration and dust formation. We publish the light curves
in a machine- readable table and encourage the use of these data by
the broader community in multiwavelength studies and modeling efforts.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 130 36 Properties of radio-observed novae (in
chronological order of discovery)
table2.dat 131 38 Overview of radio observations of the 36 novae
table3.dat 65 1935 Radio observations
refs.dat 81 76 References
appendix.dat 13 9 *Sources included in Appendix (and Table 3);
table added by CDS
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Note on appendix.dat: Some novae are observed for a few epochs at radio
wavelengths, but then observations are dropped --sometimes due to
nondetections, sometimes due to scheduling difficulties. The resulting
coverage is not sufficient to illuminate the light-curve evolution but
could be useful for future studies, so we include these data here.
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See also:
B/cb : Cataclysmic Binaries, LMXBs, and related objects (Ritter+, 2004)
II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+, 2002-2005)
V/113 : Cataclysmic Binaries, LMXBs, and related objects (Ritter+, 2003)
J/A+A/480/611 : XMM-Newton slew survey catalogue, XMMSL1 (Saxton+, 2008)
J/ApJS/187/275 : Photometric histories of recurrent novae (Schaefer, 2010)
J/AJ/140/34 : Classification of nova light curves (Strope+, 2010)
J/ApJS/197/31 : Swift X-ray obs. of classical novae. II. (Schwarz+, 2011)
J/A+A/559/A121 : U Sco outburst and pre-outburst optical sp. (Anupama, 2013)
J/MNRAS/440/3402 : Nova Cep 2013 (V809 Cep) UBVRI light curves (Munari+, 2014)
J/MNRAS/467/L31 : SS Cyg rapid radio flaring in 2016 (Mooley+, 2017)
J/AJ/154/252 : A VLA survey of magnetic CVs. I. The data (Barrett+, 2017)
J/ApJ/852/108 : Observations of gamma-ray NOVA Sco 2012 (Finzell+, 2018)
J/A+A/622/A126 : T Pyx 2011 outburst optical spectra (Pavana+, 2019)
J/A+A/639/L10 : VRI photometry of V392 Per (Munari+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Nova identifier
11- 12 I2 h RAh Hour of Right Ascension (J2000) (1)
14- 15 I2 min RAm Minute of Right Ascension (J2000)
17- 22 F6.3 s RAs Second of Right Ascension (J2000)
24 A1 --- f_Pos [a] a=Indicates position was measured using
VLA radio data presented here
26- 26 A1 --- DE- Sign of the Declination (J2000) (1)
27- 28 I2 deg DEd Degree of Declination (J2000) (1)
30- 31 I2 arcmin DEm Arcminute of Declination (J2000)
33- 37 F5.2 arcsec DEs Arcsecond of Declination (J2000)
39- 49 A11 "Y/M/D" Date Discovery Date (UT)
51- 52 A2 --- r_Date Flag on Discover (see refs.dat file)
54- 57 F4.1 mag Vmagpk [1.9/16]? Peak V band magnitude
59- 60 A2 --- r_Vmagpk Flag on Vmagpk (see refs.dat file)
62- 66 F5.1 d t2 [1/263]? Time to decline 2 magnitudes
from maximum
68- 69 A2 --- r_t2 Flag on t2 (see refs.dat file)
71- 74 F4.2 mag E(B-V) [0.06/4.3]? The (B-V) color excess
76- 79 F4.2 mag e_E(B-V) [0.01/0.2]? Uncertainty in E(B-V)
81- 82 A2 --- r_E(B-V) Flag on E(B-V) (see refs.dat file)
84- 87 I4 km/s v1 [350/2800]? Lower ejecta velocity
89- 90 A2 --- r_v1 Flag on v1 (see refs.dat file)
92- 95 I4 km/s v2 [1200/5000]? Upper ejecta velocity
97- 98 A2 --- r_v2 Flag on v2 (see refs.dat file)
100-100 A1 --- l_Dist Limit flag on Dist
101-105 F5.2 kpc Dist [0.87/12] Gaia EDR3 distance unless
otherwise noted
107-108 A2 --- r_Dist Flag on Dist (see refs.dat file)
110-113 F4.2 kpc e_Dist [0.02/4.2]? Lower uncertainty in Dist
115-118 F4.2 kpc E_Dist [0.02/6.7]? Upper uncertainty in Dist
120-127 A8 h Porb Orbital period (2)
129-130 A2 --- r_Porb Flag on Prob (see refs.dat file)
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Note (1): Coordinates "04 53 21.370 +47 21 25.84" for V392 Per are a misprint
for "04 43 21.370 +47 21 25.84"; corrected at CDS.
Note (2): In some cases, the orbital period is not known, but the nature of
the companion can be determined as main sequence (MS),
sub-giant (SG), or red giant (RG).
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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- 9 A9 --- Name Nova identifier
11- 14 I4 --- m_Name ? Year of starting observation for U Sco
16- 26 A11 --- Tel Telescope (1)
28 A1 --- f_Tel [abc] Flag on Tel (2)
30- 52 A23 --- Range Date Range of observations; YYYY MM DD-YYYY MM DD
54- 57 A4 --- f_t-t0 Limit flag on t-t0
58- 63 F6.1 d t-t0 [16.1/1697.5]? Time since discovery (3)
65 A1 --- n_t-t0 [ef] Note on t-t0 (4)
67- 70 A4 --- f_Smax Limit flag on Smax
72- 76 F5.2 mJy Smax [0.14/73]? Maximum flux density observed (3)
78 A1 --- n_Smax [ef] Note on Smax (4)
81 A1 --- Fig Figure number of optical/radio light curve
83-131 A49 --- Ref Reference or ADS bibcode
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Note (1): Telescope as follows:
VLA = the Karl G. Jansky Very Large Array, before 2010 upgrade
(14 occurrences)
Jansky VLA = the Karl G. Jansky Very Large Array, after 2010 upgrade
(14 occurrences)
ATCA = the Australia Telescope Compact Array (3 occurrences)
VLA/Merlin = VLA / MERLIN (1 occurrence)
Merlin = the Multi-Element Radio Linked Interferometer Network
(1 occurrence)
WSRT/VLA = the Westerbork Synthesis Radio Telescope / VLA (1 occurrence)
GMRT = the Giant-Meterwave Radio Telescope (1 occurrence)
Combination = Combination of telescopes, see flag (3 occurrences)
Note (2): Flag as follows:
a = NRAO Interferometer/NRAO 11m/NRAO 140ft/Bonn 100m/VLA;
b = NRAO Interferometer/NRAO 11m/NRAO 140ft/VLA;
c = WSRT/NRAO Interferometer/ARO 46m/NRAO 11m/VLA.
Note (3): Measured at C band (4-6GHz) unless it is not available
and otherwise noted.
Note (4): Flag as follows:
e = Measured at X band (8-9GHz)
f = Measured at 1.5GHz.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Nova identifier
12- 15 I4 --- m_Name ? Year of starting observation for U Sco
17- 23 F7.1 d MJD [45055/59354.3] Modified Julian Date
25- 30 F6.1 d t-t0 [0.8/1827.5] Time since discovery (1)
32- 36 F5.2 GHz Freq [0.6/43.34] Frequency
38- 38 A1 --- l_Flux The 3σ upper limit flag
39- 44 F6.2 mJy Flux [0.02/193.71] Flux density at Freq
46- 50 F5.2 mJy e_Flux [0.01/19.4] The 1σ uncertainty in Flux
52- 54 A3 --- f_Flux Flag on Flux (2)
56- 65 A10 --- Config Facility configuration (3)
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Note (1): The discovery dates are given in Table 1.
Note (2): Flag as follows:
b = Data published by Snijders et al. (1987MNRAS.228..329S 1987MNRAS.228..329S) at 1.41GHz.
c = Data also published by Bode et al. (1987MNRAS.228..217B 1987MNRAS.228..217B).
d = Data published by Taylor et al. (1987A&A...183...38T 1987A&A...183...38T).
e = Data published by Taylor et al. (1988Natur.335..235T 1988Natur.335..235T).
f = Data published by Eyres et al. (2000MNRAS.318.1086E 2000MNRAS.318.1086E).
g = Data published by Anupama et al. (2013, J/A+A/559/A121).
h = Published in Bannister et al. (2013ATEL.5685....1B 2013ATEL.5685....1B).
i = Published in Bannister et al. (2013ATEL.6058....1B 2013ATEL.6058....1B).
Note (3): The VLA configuration unless noted then either WSRT (V1370 Aql),
MERLIN (V705 Cas), GMRT (U Sco), or ATCA (V1369 Cen, V357 Mus,
V906 Car).
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Ref Reference code
4- 22 A19 --- BibCode Bibcode of the reference
24- 44 A21 --- Auth First author's name(s)
46- 81 A36 --- Comm Comment
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Byte-by-byte Description of file: appendix.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Nova identifier
11 I1 --- Nep Number of epoch of VLA observation
13 A1 --- n_Name Note on Name (1)
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Note (1): Note as follows:
a = OS And was observed with the VLA in six epochs following its 1986
eruption under programs AH185 and AH254 (PI R. Hjellming).
No confident detections were obtained.
b = QV Vul was discovered on 1987 November 15. It was observed with the VLA
in five epochs following its 1987 eruption under programs AH254 and
AH301 (PI R. Hjellming). No confident detections were obtained.
c = V5587 Sgr was observed with the Jansky VLA in three epochs following its
2011 eruption under programs VLA/10B-200 and 11A-254.
All observations yielded nondetections.
d = Following its discovery on 2011 March 27, V5588 Sgr was observed with the
Jansky VLA in six epochs under programs VLA/11A-254 and 11A-271. It shows
the start of a rise at high frequency (33GHz), while the 5.9GHz
observations yield mostly nondetections (the data are consistent with a
marginal detection on 2011 May 15). All detections were consistent with
an unresolved point source.
e = V1312 Sco was observed with the Jansky VLA in four epochs following its
2011 June 1 discovery under program VLA/11A-280. All observations yielded
nondetections.
f = Following its discovery on 2012 March 25, V2676 Oph was observed with the
Jansky VLA in four epochs under programs VLA/11B-170, 12A-479, and
12A-483. It shows the start of a rise at high frequency (33GHz), while
the 5.9GHz observation yields a marginal detection. All detections were
consistent with an unresolved point source.
g = V2677 Oph was observed with two Jansky VLA observations following its
2012 eruption under program VLA/12A-483. It was observed on 2012 June
26.5 at the C band, when it was detected with a flux density of
0.20±0.01mJy at 5.0GHz and 0.27±0.01mJy at 6.8GHz. Ka-band
observations were subsequently obtained on 2012 June 28.1 at the Ka
band, yielding a detection of 0.45±0.11mJy at 33.0GHz. Both
observations were obtained in the B configuration, and V2677 Oph
appeared as a point source.
h = V1533 Sco was observed with the Jansky VLA in two epochs following its
2013 eruption under program VLA/13A-455. The first took place on
2013 June 12.3, and the second on 2013 July 12.2; both were observed at
the C band and Ka band. All observations yielded nondetections, placing
upper limits <0.01mJy at 5.9GHz and <0.25 at 34GHz.
i = V5853 Sgr was observed with the Jansky VLA in three epochs following its
2016 August 6 discovery under program VLA/16A-318. As tabulated in
Table 3, it shows the start of a rise at high frequency (33GHz), while
the last 7GHz observation yields a marginal detection. All detections
were consistent with an unresolved point source.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 07-Mar-2022