J/ApJ/815/4 V899 Mon long-term monitoring (Ninan+, 2015)
V899 Mon: an outbursting protostar with a peculiar light curve, and
its transition phases.
Ninan J.P., Ojha D.K., Baug T., Bhatt B.C., Mohan V., Ghosh S.K.,
Men'shchikov A., Anupama G.C., Tamura M., Henning TH.
<Astrophys. J., 815, 4 (2015)>
=2015ApJ...815....4N 2015ApJ...815....4N (SIMBAD/NED BibCode)
ADC_Keywords: Equivalent widths ; Photometry, UBVRI ; Photometry, infrared ;
Stars, variable
Keywords: protoplanetary disks; stars: early-type; stars: formation;
stars: individual: V899 Mon;
stars: variables: T Tauri, Herbig Ae/Be; stars: winds, outflows
Abstract:
We present a detailed study of V899 Mon (a new member in the
FUors/EXors family of young low-mass stars undergoing outburst), based
on our long-term monitoring of the source starting from 2009 November
to 2015 April. Our optical and near-infrared photometric and
spectroscopic monitoring recorded the source transitioning from its
first outburst to a short-duration quiescence phase (<1yr), and then
returning to a second outburst. We report here the evolution of the
outflows from the inner region of the disk as the accretion rate
evolved in various epochs. Our high-resolution (R∼37000) optical
spectrum could resolve interesting clumpy structures in the outflow
traced by various lines. Change in far-infrared flux was also detected
between two outburst epochs. Based on our observations, we constrained
various stellar and envelope parameters of V899 Mon, as well as the
kinematics of its accretion and outflow. The photometric and
spectroscopic properties of this source fall between classical FUors
and EXors. Our investigation of V899 Mon hints at instability
associated with magnetospheric accretion being the physical cause of
the sudden short-duration pause of the outburst in 2011. It is also a
good candidate to explain similar short-duration pauses in outbursts
of some other FUors/EXors sources.
Description:
Our long-term optical monitoring of V899 Mon started on 2009 November
30. The observations were carried out using the 2m Himalayan Chandra
Telescope (HCT) at the Indian Astronomical Observatory, Hanle
(Ladakh), belonging to the Indian Institute of Astrophysics (IIA),
India, and the 2m telescope at the IUCAA (Inter-University Centre for
Astronomy and Astrophysics) Girawali Observatory (IGO), Girawali
(Pune), India.
Near-infrared (NIR) photometric monitoring of the source in J, H, and
K/KS bands was carried out using the HCT NIR camera (NIRCAM), the TIFR
Near Infrared Spectrometer and Imager (TIRSPEC) mounted on HCT, and
the TIFR Near Infrared Imaging Camera-II (TIRCAM2) mounted on the IGO
telescope.
Our medium-resolution (R∼1000) optical spectroscopic monitoring of
V899 Mon also started on 2009 November 30. The spectroscopic
observations were carried out using both HCT/HFOSC and IGO/IFOSC.
These observations were done in the effective wavelength range of
3700-9000Å.
We acquired a high-resolution (R∼37000) spectrum of V899 Mon during
its second outburst phase on 2014 December 22 using the Southern
African Large Telescope High Resolution Spectrograph (SALT-HRS).
NIR (1.02-2.35um) spectroscopic monitoring of V899 Mon started on 2013
September 25 using TIRSPEC mounted on HCT.
Continuum interferometric observation of V899 Mon at 1280MHz with
33.3MHz bandwidth was carried out on 2014 October 17 using the Giant
Metrewave Radio Telescope (GMRT), Pune, India.
Objects:
----------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------
06 09 19.28 -06 41 55.4 V899 Mon = V* V899 Mon
----------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 78 107 Observation log of V899 Mon
table2.dat 52 96 Magnitudes of V899 Mon
table5.dat 513 48 Spectral line measurements
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See also:
B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-2014)
J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014)
J/ApJ/778/116 : V1647 Ori long-term optical + NIR observations (Ninan+, 2013)
J/A+A/556/A60 : BVRI observations of the FUor star V582 Aur (Semkov+, 2013)
J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)
J/A+A/409/169 : UBVRI light curves of AA Tau in 1999 (Bouvier+, 2003)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 "Y/M/D" Date UT date of the observation
13- 19 I7 d JD Julian Date of the observation
21- 23 F3.1 arcsec FWHM [0.6/5.3]? Full-Width at Half-Maximum (1)
25- 58 A34 --- Setup The Filter(s) and Grism(s) used
60- 78 A19 --- Inst Instrument(s) used (HFOSC, IFOSC, TIRSPEC,
NIRCAM or TIRCAM2);
see the "Description" section above
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Note (1): This is a measure of the seeing.
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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- 7 I7 d JD Julian Date of the observation
9- 13 F5.2 mag Umag [16.5/16.6]? The U band magnitude (1)
15- 19 F5.2 mag Bmag [15.75]? The B band magnitude (1)
21- 25 F5.2 mag Vmag [13.1/16.9]? The V band magnitude (1)
27- 31 F5.2 mag Rmag [12.1/15.8]? The R band magnitude (1)
33- 37 F5.2 mag Imag [11.1/14.8]? The I band magnitude (1)
39- 42 F4.2 mag Jmag [9/10]? The J band magnitude (1)
44- 47 F4.2 mag Hmag [7.9/8.9]? The H band magnitude (1)
49- 52 F4.2 mag Kmag [7.1/8.2]? The KS band magnitude (1)
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Note (1): Errors on U, B, V, R and I magnitudes are <0.02mag, TIRSPEC
J, H and KS magnitudes have errors <0.02mag, and TIRCAM2 and
NIRCAM J, H, K magnitudes have errors <0.06mag.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "Y/M/D" Date UT date of the observation
12- 21 F10.2 d JD Julian Date of the observation
23- 28 F6.2 0.1nm EWHa [-64.5/-6.8]? Hα λ6562.8
equivalent width (1)
30- 37 E8.2 mW/m2 FHa ? Hα λ6562.8 flux (2)
39- 43 F5.3 0.1nm EWaHa [0/7.2]? Hα λ6562.8 absorption
equivalent width (1)
45- 48 I4 km/s VHa ? Hα λ6562.8 outflow velocity
50- 55 F6.2 0.1nm EWCaII1 ? Ca II λ8498 equivalent width (1)
57- 64 E8.2 mW/m2 FCaII1 ? Ca II λ8498 flux (2)
66- 71 F6.2 0.1nm EWCaII2 ? Ca II λ8542 equivalent width (1)
73- 80 E8.2 mW/m2 FCaII2 ? Ca II λ8542 flux (2)
82- 86 F5.3 0.1nm EWaCaII2 [0.4/3.8]? Ca II λ8542 absorption
equivalent width (1)
88- 91 I4 km/s VCaII2 ? Ca II λ8542 outflow velocity
93- 97 F5.2 0.1nm EWCaII3 ? Ca II λ8662 equivalent width (1)
99-106 E8.2 mW/m2 FCaII3 ? Ca II λ8662 flux (2)
108-112 F5.3 0.1nm EWaCaII3 [0/1.7]? Ca II λ8662 absorption
equivalent width (1)
114-119 F6.1 km/s VCaII3 ? Ca II λ8662 outflow velocity
121-126 F6.2 0.1nm EWOI1 ? [O I] λ6300.3 equivalent width (1)
128-135 E8.2 mW/m2 FOI1 ? [O I] λ6300.3 flux (2)
137-143 F7.3 0.1nm EWOI2 ? [O I] λ6363.8 equivalent width (1)
145-152 E8.2 mW/m2 FOI2 ? [O I] λ6363.8 flux (2)
154-158 F5.3 0.1nm EWOI3 ? O I λ7773 equivalent width (1)
160-168 E9.2 mW/m2 FOI3 ? O I λ7773 flux (2)
170-173 F4.2 0.1nm EWH8 ? H8 λ3889.0 equivalent width (1)
175-183 E9.2 mW/m2 FH8 ? H8 λ3889.0 flux (2)
185-188 F4.2 0.1nm EWH7 ? H7 λ3970.1 equivalent width (1)
190-198 E9.2 mW/m2 FH7 ? H7 λ3970.1 flux (2)
200-203 F4.2 0.1nm EWHd [1.6/4.3]? Hδ λ4101.7
equivalent width (1)
205-213 E9.2 mW/m2 FHd ? Hδ λ4101.7 flux (2)
215-218 F4.2 0.1nm EWHg [2.4/4.3]? Hγ λ4340.5
equivalent width (1)
220-228 E9.2 mW/m2 FHg ? Hγ λ4340.5 flux (2)
230-233 F4.2 0.1nm EWHb [1.1/4.4]? Hβ λ4861.3
equivalent width (1)
235-243 E9.2 mW/m2 FHb ? Hβ λ4861.3 flux (2)
245-248 F4.2 0.1nm EWaHb [1/5]? Hβ λ4861.3 absorption
equivalent width (1)
250-255 F6.1 km/s VHb ? Hβ λ4861.3 outflow velocity
257-262 F6.2 0.1nm EWCaIIK [-15.5/2.1]? CaII(K) λ3933.6
equivalent width (1)
264-272 E9.2 mW/m2 FCaIIK ? CaII(K) λ3933.6 flux (2)
274-278 F5.2 0.1nm EWSII1 ? [S II] λ4069 equivalent width (1)
280-287 E8.2 mW/m2 FSII1 ? [S II] λ4069 flux (2)
289-294 F6.3 0.1nm EWFeII1 ? [Fe II] λ4815 equivalent width (1)
296-303 E8.2 mW/m2 FFeII1 ? [Fe II] λ4815 flux (2)
305-309 F5.3 0.1nm EWHeI ? He I λ5015.6 equivalent width (1)
311-319 E9.2 mW/m2 FHeI ? He I λ5015.6 flux (2)
321-324 F4.2 0.1nm EWNaI ? Na D λ5895 equivalent width (1)
326-334 E9.2 mW/m2 FNaI ? Na D λ5895 flux (2)
336-341 F6.3 0.1nm EWFeII2 ? Fe II λ6432 equivalent width (1)
343-350 E8.2 mW/m2 FFeII2 ? Fe II λ6432 flux (2)
352-357 F6.3 0.1nm EWFeII3 ? Fe II λ6517 equivalent width (1)
359-366 E8.2 mW/m2 FFeII3 ? Fe II λ6517 flux (2)
368-373 F6.3 0.1nm EWSII2 ? [S II] λ6730 equivalent width (1)
375-382 E8.2 mW/m2 FSII2 ? [S II] λ6730 flux (2)
384-389 F6.3 0.1nm EWFeII4 ? [Fe II] λ7155 equivalent width (1)
391-398 E8.2 mW/m2 FFeII4 ? [Fe II] λ7155 flux (2)
400-405 F6.3 0.1nm EWCaII4 ? [Ca II] λ7291 equivalent width (1)
407-414 E8.2 mW/m2 FCaII4 ? [Ca II] λ7291 flux (2)
416-421 F6.3 0.1nm EWBlend [-2.6/-0.2]? [OI]+[CaII] λ7324
equivalent width (1)
423-430 E8.2 mW/m2 FWBlend ? [OI]+[CaII] λ7324 flux (2)
432-437 F6.3 0.1nm EWFeII5 ? [Fe II] λ7380 equivalent width (1)
439-446 E8.2 mW/m2 FFeII5 ? [Fe II] λ7380 flux (2)
448-454 F7.4 0.1nm EWKI ? K I λ7699 equivalent width (1)
456-464 E9.2 mW/m2 FKI ? K I λ7699 flux (2)
466-471 F6.3 0.1nm EWFeI ? Fe I λ8388 equivalent width (1)
473-480 E8.2 mW/m2 FFeI ? Fe I λ8388 flux (2)
482-487 F6.3 0.1nm EWOI4 ? O I λ8446 equivalent width (1)
489-497 E9.2 mW/m2 FOI4 ? O I λ8446 flux (2)
499-504 F6.3 0.1nm EWFeII6 ? [Fe II] λ8616 equivalent width (1)
506-513 E8.2 mW/m2 FFeII6 ? [Fe II] λ8616 flux (2)
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Note (1): In units of Angstroms.
Note (2): In units of erg/s/cm-2.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 04-Mar-2016