J/ApJ/852/108 Multiwavelength obs. of gamma-ray NOVA Sco 2012 (Finzell+, 2018)
A detailed observational analysis of V1324 Sco, the most gamma-ray-luminous
classical nova to date.
Finzell T., Chomiuk L., Metzger B.D., Walter F.M., Linford J.D., Mukai K.,
Nelson T., Weston J.H.S., Zheng Y., Sokoloski J.L., Mioduszewski A.,
Rupen M.P., Dong S., Starrfield S., Cheung C.C., Woodward C.E., Taylor G.B.,
Bohlsen T., Buil C., Prieto J., Wagner R.M., Bensby T., Bond I.A., Sumi T.,
Bennett D.P., Abe F., Koshimoto N., Suzuki D., Tristram P.J., Christie G.W.,
Natusch T., McCormick J., Yee J., Gould A.
<Astrophys. J., 852, 108 (2018)>
=2018ApJ...852..108F 2018ApJ...852..108F
ADC_Keywords: Novae; Photometry, UBVRI; Radio continuum; Spectra, optical
Keywords: gamma rays: stars ; novae, cataclysmic variables ;
radio continuum: stars ; stars: individual (V1324 Sco)
Abstract:
It has recently been discovered that some, if not all, classical novae
emit GeV gamma-rays during outburst, but the mechanisms involved in
the production of gamma-rays are still not well understood. We present
here a comprehensive multiwavelength data set-from radio to X-rays-for
the most gamma-ray-luminous classical nova to date, V1324 Sco. Using
this data set, we show that V1324 Sco is a canonical dusty FeII-type
nova, with a maximum ejecta velocity of 2600km/s and an ejecta mass of
a few x10-5M☉. There is also evidence for complex shock
interactions, including a double-peaked radio light curve which shows
high brightness temperatures at early times. To explore why V1324 Sco
was so gamma-ray luminous, we present a model of the nova ejecta
featuring strong internal shocks and find that higher gamma-ray
luminosities result from higher ejecta velocities and/or mass-loss
rates. Comparison of V1324 Sco with other gamma-ray-detected novae
does not show clear signatures of either, and we conclude that a
larger sample of similarly well-observed novae is needed to understand
the origin and variation of gamma-rays in novae.
Description:
V1324 Sco falls within one of the fields that the Microlensing
Observations in Astrophysics collaboration (MOA; Wagner+
2012ATel.4157....1W 2012ATel.4157....1W) continually observes with the MOAII 1.8m
telescope at Mt. Johns Observatory in New Zealand. V1324 Sco was
initially detected in 2012 April by their high-cadence I-band
photometry. We take 2012 June 1 to be day 0, or the start of the nova
outburst.
Apart from the standard I broadband filter, the MicroFUN group
(http://www.astronomy.ohio-state.edu/~microfun/) follow-up
observations also used V and I Bessel filters. Other observations were
made in B, V, and I filters using the Small & Moderate Aperture
Research Telescope System (SMARTS) 1.3m telescope and Auckland
Observatories.
Along with the MOA and MicroFUN data, we also present multicolor
photometry from Fred Walter's ongoing Stony Brook/SMARTS Atlas of
(mostly) Southern Novae (see Walter+ 2012PASP..124.1057W 2012PASP..124.1057W for further
information on this data set), as well as data from the American
Association of Variable Star Observers (AAVSO). The SMARTS data use
the ANDICAM instrument on the 1.3m telescope and provide both optical
(B, V, R, I) and near-IR (J, H, K) filters going from day +35 to day
+124, while the AAVSO data use optical (V, B, R) filters and go from
day +7 to day +445.
Finally, we incorporate the UV data taken contemporaneously with the
X-ray observations. The UV data come from the Ultraviolet/Optical
Telescope (UVOT) on board Swift. Each observation was taken using the
UVM2 filter, which is centered on 2246Å.
See Table 1 for the UV-Opt-IR data.
We obtained sensitive radio observations (spanning 2012 Jun to 2014
Dec) of V1324 Sco between 2012 June 26 and 2014 December 19 with the
Karl G. Jansky Very Large Array (VLA) through programs S4322, 12A-483,
12B-375, 13A-461, 13B-057, and S61420 (coverage from 4 to 37GHz).
See section 3.
All spectroscopic observations (spanning 2012 Jun to 2013 Aug) taken
with the VLT/UVES, Vixen/LISA, SMARTS 1.5m, MIKE, LBT/MODS1 or
SOAR/Goodman, are listed in Table 3. See section 4.
Multiple X-ray observations were made using the Swift X-ray Telescope
(XRT), all of them yielding non-detections. See section 5.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
17 50 53.91 -32 37 21.1 V* V1324 Sco = NOVA Sco 2012
----------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 69 13132 Table of photometric data
table2.dat 106 21 VLA observations of V1324 Sco
table3.dat 70 17 Optical spectroscopic observations
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See also:
B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-2014)
B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)
J/A+A/459/875 : Early spectral evolution of Nova Sgr 2004 (Ederoclite+, 2006)
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/MNRAS/435/771 : Nova Mon 2012 BV(RI)c light curves (Munari+, 2013)
J/A+A/554/A123 : Near-IR catalog of novae in VVV survey area (Saito+, 2013)
J/A+A/566/A120 : 3D dust extinction in Milky Way bulge (Schultheis+, 2014)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/ApJ/834/107 : Follow-up photometry of M101 OT2015-1 (Blagorodnova+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 "Y/M/D" Date UT date of the observation
13- 23 F11.3 d JD Julian Date of the observation
25- 33 F9.3 d t-t0 [-2413.2/446] Days relative to 2012 June 1
35- 38 A4 --- Filt Filter used (I, V, B, R, J, K, H or UVM2)
40- 44 F5.2 mag mag [4.6/25.2] Observed magnitude in Filter
46- 49 F4.2 mag e_mag [0/5] Uncertainty in mag
51- 57 A7 --- Obs Observer/Group identifier (1)
59- 69 A11 --- Tel Telescope information (2)
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Note (1): Observer/Group identifier as follows:
MOA = Microlensing Observations in Astrophysics collaboration
(12409 occurrences);
AAVSO = American Association of Variable Star Observers
(610 occurrences);
Walter = Walter+ 2012PASP..124.1057W 2012PASP..124.1057W (107 occurrences)
Swift = Swift/UVOT (6 occurrences).
Note (2): Telescope information as follows:
AUCK-B = Auckland Observatory B band (82 occurrences);
AUCK-I = Auckland Observatory I band (95 occurrences);
AUCK-V = Auckland Observatory V band (97 occurrences);
MJUO-B = Mt. John University Observatory B band; (68 occurrences)
MJUO-I = Mt. John University Observatory I band (1037 occurrences);
MJUO-Ibroad = Mt. John University Observatory broad I band (10571 occurrences);
MJUO-V = Mt. John University Observatory V band (215 occurrences);
SMARTS = CTIO SMARTS 1.3m (351 occurrences);
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 F6.1 d JD Julian date; JD-2450000
8- 18 A11 "date" Date UT date of observation
20- 24 F5.1 d t-t0 [25/930] Days since t0 (= 2012 June 1)
26- 28 A3 --- Conf VLA configuration
30 A1 --- l_F4.5GHz Limit flag on F4.5GHz (1)
32- 36 F5.3 mJy F4.5GHz [0.1/1.4]? VLA 4.5GHz flux
38- 42 F5.3 mJy e_F4.5GHz [0.02/0.3]? F4.5GHz uncertainty
44- 48 F5.3 mJy F7.8GHz [0.1/3]? VLA 7.8GHz flux
50- 54 F5.3 mJy e_F7.8GHz [0.02/0.2]? F7.8GHz uncertainty
56- 60 F5.3 mJy F13.3GHz [0.2/3]? VLA 13.3GHz flux
62- 66 F5.3 mJy e_F13.3GHz [0.04/0.4]? F13.3GHz uncertainty
68- 72 F5.3 mJy F17.4GHz [0.2/4.1]? VLA 17.4GHz flux
74- 78 F5.3 mJy e_F17.4GHz [0.04/0.5]? F17.4GHz uncertainty
80 A1 --- l_F27.5GHz Limit flag on F27.5GHz (1)
82- 86 F5.3 mJy F27.5GHz [0.2/5.7]? VLA 27.5GHz flux
88- 92 F5.3 mJy e_F27.5GHz [0.1/0.8]? F27.5GHz uncertainty
94 A1 --- l_F36.5GHz Limit flag on F36.5GHz (1)
96-100 F5.3 mJy F36.5GHz [0.3/7]? VLA 36.5GHz flux
102-106 F5.3 mJy e_F36.5GHz [0.1/1]? F36.5GHz uncertainty
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Note (1): Detections are defined as flux >5σ. Non-detections are given
as the 5σ upper limits.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 "Y/M/D" Date UT date of observation
15- 20 F6.1 d t-t0 [3/450] Days since t0 (= 2012 June 1)
22- 28 A7 --- Obs Observer
30- 44 A15 --- Tel Telescope
46- 52 A7 --- Inst Instrument
54 A1 --- u_Disp [~] Uncertainty flag on Disp
55- 59 F5.3 0.1nm Disp Dispersion in Angstroms
61- 64 I4 0.1nm lam1 [3000/5620] Minimum wavelength range in Angstroms
65 A1 --- --- [-]
66- 70 I5 0.1nm lam2 [5420/10000] Maximum wavelength range in Angstroms
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 19-Sep-2018