scholarly journals UV spectroscopy confirms SU Lyn to be a symbiotic star

2020 ◽  
Vol 500 (1) ◽  
pp. L12-L16
Author(s):  
Vipin Kumar ◽  
Mudit K Srivastava ◽  
Dipankar P K Banerjee ◽  
Vishal Joshi
Keyword(s):  
Near Infrared ◽  
Uv Spectroscopy ◽  
Symbiotic Star ◽  
Symbiotic Stars ◽  
High Excitation ◽  
Uv Spectrum ◽  
Infrared Observations ◽  
X Ray ◽  
The Galaxy ◽  
Type Giant

ABSTRACT SU Lyn, a star that ostensibly appears to be an unremarkable late M type giant, has recently been proposed to be a symbiotic star largely based on its hard X-ray properties. The star does not display, in low-resolution optical spectra, the high excitation lines typically seen in the spectra of symbiotic stars. In this work, ultraviolet (UV), optical, and near-infrared observations are presented, aimed at exploring and strengthening the proposed symbiotic classification for this star. Our far-UV 1300–1800 Å spectrum of SU Lyn, obtained with the ASTROSAT mission’s UVIT payload, shows emission lines of Si iv, C iv, O iii, and N iii in a spectrum typical of symbiotic stars. The UV spectrum robustly confirms SU Lyn’s symbiotic nature. The detection of high excitation lines in a high-resolution optical spectrum further consolidates its symbiotic nature. As is being recognized, the potential existence of other similar symbiotic systems could significantly impact the census of symbiotic stars in the Galaxy.

scholarly journals X-Ray and Ultraviolet Observations of AG Draconis during Quiescence and Outburst

1987 ◽  
Vol 93 ◽  
pp. 763-763
Author(s):  
A. Cassatella ◽  
F.A. Córdova ◽  
M. Friedjung ◽  
J. Kenyom ◽  
L. Piro ◽  
...  
Keyword(s):  
Orbital Motion ◽  
Uv Light ◽  
Low Energy ◽  
Emission Lines ◽  
Symbiotic Star ◽  
Symbiotic Stars ◽  
Uv Spectrum ◽  
X Ray ◽  
High Ionization ◽  
Ultraviolet Observations

AbstractWe describe the first X-ray monitoring of a symbiotic star during phases of enhanced activity. AG Dra is a Pop II object with a composite spectrum, characterized by a cool K-type component, prominent high ionization emission lines and a strong UV continuum which is attributed to a hot dwarf companion. Periodic variability of the UV radiation during minimum could be attributed to the orbital motion of the system. In April 1980 HEAO-2 detected an intense, soft X-ray flux from AG Dra, stronger than in other symbiotic stars. After one major outburst of November 1980, which continued until 1983, two more outbursts occurred in February 1985 and January 1986, and coordinated X-ray (EXOSAT) and ultraviolet (IUE) observations were organized to study the behaviour of AG Dra during different activity phases. EXOSAT observations made during decline after the 1985 outburst, revealed a weak X-ray flux in the Thin Lexan filter of the Low Energy dedtector. Observations made during minimum, in June and November 1985, at phases 0.22 and 0.50 of the UV light curve, disclosed the presence of an intense X-ray flux, which was not occulted in November. AG Dra was again observed with EXOSAT in February 1986 when the stellar luminosity was still at maximum. No X-ray flux was detected, in spite of the prominent, high ionization UV spectrum observed with IUE.A detailed discussion of the X-ray and ultraviolet results on AG Dra in the light of possible models is in progress.

Near-Infrared Observations of a Type-2 QSO at z = 0.9

1999 ◽  
Vol 186 ◽  
pp. 361-361
Author(s):  
K. Nakanishi ◽  
M. Akiyama ◽  
K. Ohta ◽  
T. Yamada
Keyword(s):  
Optical Spectrum ◽  
Near Infrared ◽  
High Excitation ◽  
Infrared Observations ◽  
X Ray ◽  
High Ionization ◽  
Deep Survey

We report the results of near-infrared observations of a type-2 QSO, AX J08494+4454 at z = 0.9 which was identified in our optical follow-up observations of the ASCA Lynx deep survey. This object has a hard X-ray spectrum with an X-ray luminosity of about 1×1044 erg s−1 in 2–10 keV. The optical spectrum shows high-excitation and high-ionization lines but no significant broad Hβ emission. These properties strongly suggest that this object is a “type-2” QSO (Ohta et al. 1996).

scholarly journals Infrared Analysis of Supernova Remnants

1988 ◽  
Vol 101 ◽  
pp. 363-378 ◽  
Author(s):  
Eli Dwek
Keyword(s):  
Supernova Remnants ◽  
Infrared Emission ◽  
Infrared Analysis ◽  
Atomic Processes ◽  
Infrared Observations ◽  
X Ray ◽  
Physical Conditions ◽  
The Galaxy ◽  
Dust Grain ◽  
Astronomical Satellite

AbstractInfrared observations of supernova remnants obtained with the Infrared Astronomical Satellite provide new insights into the dynamics and energetics of the remnants, and into their interaction with the ambient interstellar medium. In most remnants the infrared emission arises from dust that is collisionally heated by the X-ray emitting gas. The infrared observations can therefore be used as a diagnostic for the physical conditions of the shocked gas. In particular, it is shown that all the prominent X-ray remnants in the Galaxy and in the LMC cool mainly by dust grain collisions instead of atomic processes.

The nova type outburst of the symbiotic star AS 296

1990 ◽  
Vol 122 ◽  
pp. 440-441
Author(s):  
Ulisse Munari
Keyword(s):  
Orbital Period ◽  
Active Phase ◽  
Borderline Case ◽  
Symbiotic Star ◽  
Symbiotic Stars ◽  
Late Type ◽  
Type Giant ◽  
One Year

AbstractThe photometric and spectroscopic evolutions, displayed by AS 296 since the June 1988 outburst ([1]), are presented and discussed. The main features of the model outlined by [2], [3] and [4], are confirmed and further developped. An orbital period of about 3 years is inferred from Hα modulation (see [5]).The outburst originated from a TNR event in the accreted envelope of a WD. The IUE and optical spectroscopic evolution agrees with the expected scenario for degenerate conditions in the accreted material, while the high quiescence luminosity of the WD would indicate nondegenerate conditions.The late type giant passed unchanged the outburst. Also the region of Hα formation was not touched by the eruption.After one year the system has not yet reached the quiescence again. The photometric evolution displayed by AS 296 up to June 15, 1989 is presented in Fig.1.In Tab.1, the main features exhibited by symbiotic stars that have experienced a TNR event are summarized. The first 8 objects in the table are usually collectively called "symbiotic novae". They distinguish themselves for the very long outburst duration. At present, AS 296 appears to be a borderline case of such class, and a firm understanding needs to wait for the end of current active phase.

scholarly journals X-RAY AND NEAR-INFRARED OBSERVATIONS OF THE OBSCURED ACCRETING PULSAR IGR J18179–1621

2012 ◽  
Vol 757 (2) ◽  
pp. 143 ◽  
Author(s):  
M. A. Nowak ◽  
A. Paizis ◽  
J. Rodriguez ◽  
S. Chaty ◽  
M. Del Santo ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Observations ◽  
X Ray

scholarly journals Chandra X-ray and Gemini near-infrared observations of the eclipsing millisecond pulsar SWIFT J1749.4−2807 in quiescence

2012 ◽  
Vol 429 (1) ◽  
pp. 523-528 ◽  
Author(s):  
Peter G. Jonker ◽  
Manuel A. P. Torres ◽  
Danny Steeghs ◽  
Deepto Chakrabarty
Keyword(s):  
Near Infrared ◽  
Millisecond Pulsar ◽  
Infrared Observations ◽  
X Ray

Deep Near‐Infrared Observations of the X‐Ray–emitting Class 0 Protostar Candidates in the Orion Molecular Cloud 3

2002 ◽  
Vol 573 (1) ◽  
pp. 270-274 ◽  
Author(s):  
Masahiro Tsujimoto ◽  
Katsuji Koyama ◽  
Yohko Tsuboi ◽  
George Chartas ◽  
Miwa Goto ◽  
...  
Keyword(s):  
Molecular Cloud ◽  
Near Infrared ◽  
Infrared Observations ◽  
X Ray

scholarly journals Near infrared observations of soft X-ray selected AGN

2002 ◽  
Vol 386 (3) ◽  
pp. 854-859 ◽  
Author(s):  
D. Grupe ◽  
H.-C. Thomas
Keyword(s):  
Near Infrared ◽  
Infrared Observations ◽  
X Ray

scholarly journals Summary of Final Discussion

1988 ◽  
Vol 103 ◽  
pp. 347-348
Author(s):  
Robert E. Stencel
Keyword(s):  
Near Infrared ◽  
Recent History ◽  
Radio Observations ◽  
Infrared Observations ◽  
X Ray ◽  
History Of

The last session of the Colloquium was Chaired by Harry Nussbaumer and opened with statements from members of a panel comprised of Livio, Mikolajewska, Luud, Viotti, Magalliaes, Slovak, Kwok and Whitelock. Viotti began by comparing the available data for symbiotics historically and since IAU Colloquium 70 in 1981. He emphasized new UV, X-ray, infrared and radio observations. He also sketched the recent history of wavelength specific publications. Whitelock stated that it now seems clear all D-types probably contain Miras and that S-types do not evolve into D-types. Luud stated that his group intends to continue its near infrared observations with the 2 meter at Tartu, and that it is important to confirm conclusions based on IRAS data. He mentioned that masses for the Miras are needed given the discrepancy between observed and evolutionary masses.

scholarly journals Broad view on hard X-ray background emission of the Galaxy

2009 ◽  
Vol 5 (H15) ◽  
pp. 810-810
Author(s):  
Roman Krivonos ◽  
Mikhail Revnivtsev ◽  
Sergey Tsygankov ◽  
Eugene Churazov ◽  
Rashid Sunyaev
Keyword(s):  
Near Infrared ◽  
Galactic Disk ◽  
Broad Band ◽  
Point Sources ◽  
X Rays ◽  
X Ray ◽  
Scientific Debate ◽  
The Galaxy ◽  
Background Emission ◽  
Galactic Background

AbstractThe nature of the Galactic Ridge X-Ray Emission (GRXE) has been under scientific debate since its discovery more than 30 years ago. It is observed as extended emission along the Galactic disk. The question was: is GRXE truly diffuse or is it composed from a large number of unresolved point sources? Using near-infrared Galaxy maps measured with the DIRBE experiment and data from the INTEGRAL observatory, we show that the galactic background in the energy range 20-60 keV originates from the stellar population of the Galaxy, which is in contrast to the diffuse nature believed before (Krivonos et al., 2007). Here we show preliminary results of studying the transition region from hard X-rays to gamma diffuse background of the Galaxy, revealing the broad band picture of Galactic Background emission.

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