[RP2006] 774

SUSPECTED LMC   Equatorial coordinates α =  83.165399 ± 0.259800 | 05 32 39.690174 δ =  -69.513745 ± 0.308600 | -69 30 49.483082   Constellation Dorado Symbiotic IR Type D’🡕 Source: Akras, S., Guzman-Ramirez, L., Leal-Ferreira, M. L., et al., 2019, ApJS, 240, 21, 2019ApJS..240…21A Spectral Type   Magnitude range (V)   Outbursts No

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Identifiers

[RP2006] 774	GSC –	TYC –	WRAY –
SIMBAD [RP2006] 774	HIP –	SAO –	Hen –
BD –	IRAS –	GAIA DR2 4658034080040925568	ESO –
HD –	2MASS J05323971-6930494	WISE J053239.70-693049.3	AAVSO –

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Position

Right ascension (°)	83.165399 ± 0.259800  refGaia Collaboration, Brown, A. G. A., Vallenari, A., et al., 2018, A&A, 616, A1, 2018A&A…616A…1G	Parallax (mas)	–	Reddening E(B-V) (mag)	0.396 ± 0.144refSchlafly, E. F., Finkbeiner, D. P., 2011, ApJ, 737, 103, 2011ApJ…737..103S
Declination (°)	-69.513745 ± 0.308600refGaia Collaboration, Brown, A. G. A., Vallenari, A., et al., 2018, A&A, 616, A1, 2018A&A…616A…1G	Distance (kpc)	49.97 ± 0.19refPietrzyński, G., Graczyk, D., Gieren, W., et al., 2013, Nature, 495, 76, 2013Natur.495…76P
Galactic longitude (°)	280.028253 ± 0.308600refGaia Collaboration, Brown, A. G. A., Vallenari, A., et al., 2018, A&A, 616, A1, 2018A&A…616A…1G	Proper motion in α (mas/yr)	1.855 ± 0.515refGaia Collaboration, Brown, A. G. A., Vallenari, A., et al., 2018, A&A, 616, A1, 2018A&A…616A…1G
Galactic latitude (°)	-32.148368 ± 0.259800refGaia Collaboration, Brown, A. G. A., Vallenari, A., et al., 2018, A&A, 616, A1, 2018A&A…616A…1G	Proper motion in δ (mas/yr)	0.027 ± 0.833refGaia Collaboration, Brown, A. G. A., Vallenari, A., et al., 2018, A&A, 616, A1, 2018A&A…616A…1G

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Observations

U (mag)	18.42refMiszalski, B., Napiwotzki, R., Cioni, M. R. L., et al., 2011, A&A, 531, A157,2011A&A…531A.157M	X-Ray		Flickering
B (mag)	18.78refMiszalski, B., Napiwotzki, R., Cioni, M. R. L., et al., 2011, A&A, 531, A157,2011A&A…531A.157M	X-Ray type		Outbursts	No
V (mag)	17.92refMiszalski, B., Napiwotzki, R., Cioni, M. R. L., et al., 2011, A&A, 531, A157,2011A&A…531A.157M	IUE	No	Type
R (mag)		IRAS flux at 12 μm (Jy)		IPmax (eV)
I (mag)	17.40refZaritsky, D., Harris, J., Thompson, I. B., et al., 2004, AJ, 128, 1606, 2004AJ….128.1606Z	IRAS flux at 25 μm (Jy)		OVI lines
G (mag)	18.84refGaia Collaboration, Brown, A. G. A., Vallenari, A., et al., 2018, A&A, 616, A1, 2018A&A…616A…1G	IRAS flux at 60 μm (Jy)
J (mag)	16.97refCutri, R. M., Skrutskie, M. F., van Dyk, S., et al., 2012, VizieR Online Data Catalog: II/281,2012yCat.2281….0C	IRAS flux at 100 μm (Jy)
H (mag)	16.04refCutri, R. M., Skrutskie, M. F., van Dyk, S., et al., 2012, VizieR Online Data Catalog: II/281,2012yCat.2281….0C	WISE W1 (mag)	12.29refCutri, R. M., et al., 2014, I II/328, 2014yCat.2328….0C
K (mag)	14.93refCutri, R. M., Skrutskie, M. F., van Dyk, S., et al., 2012, VizieR Online Data Catalog: II/281,2012yCat.2281….0C	WISE W2 (mag)	11.25refCutri, R. M., et al., 2014, I II/328, 2014yCat.2328….0C
L (mag)		WISE W3 (mag)	7.51refCutri, R. M., et al., 2014, I II/328, 2014yCat.2328….0C
		WISE W4 (mag)	5.34refCutri, R. M., et al., 2014, I II/328, 2014yCat.2328….0C
		Radio
		Radio flux (mJy)

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Orbit

Orbital period (days)		γ velocity (km/h)		Size of giant’s orbit (AU)
Eccentricity		RV of giant (km/h)		Separation (AU)
Inclination (°)		Inferior conj. of giant (JD)		Mass function
Ephemeris type				Mass ratio
Ephemeris T0 (JD)

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Cool component

Spectral type		Mass (M⊙)		Pulsation
Eff. temperature (K)		Radius (R⊙)		Type
IR type	D’🡕 Source: Akras, S., Guzman-Ramirez, L., Leal-Ferreira, M. L., et al., 2019, ApJS, 240, 21, 2019ApJS..240…21A, refAkras, S., Guzman-Ramirez, L., Leal-Ferreira, M. L., et al., 2019, ApJS, 240, 21, 2019ApJS..240…21A	Luminosity (L⊙)		Pulsation period (days)
Metallicity [Fe/H]				Ephemeris type
				Ephemeris T0 (JD)

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Hot component

Type/Spectra		Mass (M⊙)		Spin period (min)
Eff. temperature (K)		Radius (R⊙)		Accretion disk
Lower limit (K)		Luminosity (L⊙)
Upper limit (K)

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Links

SIMBAD     CDS Portal

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Notes

The star appears to have significant nebular Hα emission and the NIR and MIR properties suggest an obscured RGB (or possibly AGB) star. The OGLE-III lightcurve of [RP2006] 774 appears to show low-amplitude semi-regular variability on the order of ∼40–80 days and this could be attributed to an RGB star (Miszalski et al., 2011). Reid (2014) did not consider the MIR SED steep enough for a symbiotic star and classified it as YSO.

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References

• Akras, S., Guzman-Ramirez, L., Leal-Ferreira, M. L., et al., 2019, ApJS, 240, 21, 2019ApJS..240…21A
• Miszalski, B., Napiwotzki, R., Cioni, M. R. L., et al., 2011, A&A, 531, A157, 2011A&A…531A.157M
• Reid, W. A., 2014, MNRAS, 438, 2642, 2014MNRAS.438.2642R

Last updated: May 2, 2019 @ 11:20 am