New Online Database of Symbiotic Variables: LL Cas

Constellation
Cassiopeia

Equatorial coordinates
α = 23 09 20.162
δ = +54 44 50.035

Galactic coordinates
l = 108.4688°
b = -5.2318°

Suspected	1974^Ref
Confirmed	1992^Ref
Symbiotic IR type	S^Ref
Hot component type	shell-burning^Ref
Outbursts	-

Identifiers

LL Cas	IRAS -	GSC2.4.2 N1CK029506	AAVSO 000-BCV-194
SIMBAD V* LL Cas	Pan-STARRS 173693473339587596	SAO -	VSX 6591
GAIA DR3 1996657659424174592	SkyMapper -	WRAY -	GCVS LL Cas
2MASS J23092015+5444500	HIP -	Hen -	BD -
WISE J230920.15+544450.0	TYC -	ESO -	HD -

Symbiotic Catalogs

Bidelman (1954)	-	Allen (1984)	-	Belzcyński et al. (2001)	LL Cas (Conf.)
Gaposchkin (1957)	-	Kenyon (1986)	-	Akras et al. (2019)	LL Cas (Conf.)
Boyarchuk (1969)	-	Vaidis (1988, 1991)	-

Position

Right ascension (°)	347.3340^Ref	Parallax (mas)	0.060±0.053^Ref	Reddening E(B-V) (mag)	0.36±0.01^Ref ^{, Note}
Declination (°)	54.7472^Ref	Distance (kpc)	10^Ref 6.51^Ref ^{, Note}, 6.20^Ref ^{, Note}
Galactic longitude (°)	108.4688^Ref	Proper motion in α (mas/yr)	-1.47±0.06^Ref
Galactic latitude (°)	-5.2318^Ref	Proper motion in δ (mas/yr)	-0.65±0.05^Ref

Observations

X-Ray	No^Ref	IR type	S^Ref	Radio	Yes^Ref
X-Ray type	-	J (mag)	8.49^Ref	Flickering	-
GALEX FUV (mag)	-	H (mag)	7.56^Ref	Outbursts	-
GALEX NUV (mag)	-	K (mag)	7.13^Ref	Outburst type	-
IUE	No^Ref	WISE W1 (mag)	6.77^Ref	Jets	-
FUSE	No^Ref	WISE W2 (mag)	6.57^Ref	Resolved nebula	-
U (mag)	-	WISE W3 (mag)	6.01^Ref	IPmax (eV)	99^Ref
B (mag)	-	WISE W4 (mag)	5.89^Ref	[O III] lines	Yes^Ref
V (mag)	-	IRAS 12μm (Jy)	-	He II lines	Yes^Ref
R (mag)	-	IRAS 25μm (Jy)	-	[Fe VII] lines	Yes^Ref
I (mag)	-	IRAS 60μm (Jy)	-	O VI lines	No^Ref
BP (mag)	15.55^Ref	IRAS 100μm (Jy)	-
G (mag)	13.48^Ref	AKARI S09 (Jy)	0.18^Ref
RP (mag)	11.60^Ref	AKARI S18 (Jy)	-

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	-
Eclipses	-			Mass ratio	2.5^Ref
Orbital ephemeris	-

Cool component

Spectral type	M2^Ref	Mass (M_⊙)	<1.5^Ref	Pulsation	Yes^Ref
Eff. temperature (K)	-	Radius (R_⊙)	-	Type	Mira^Ref
IR type	S^Ref	Luminosity (L_⊙)	-	Pulsation period (days)	286.6^Ref, 283.02^Ref, 284.2^Ref
Metallicity [Fe/H]	-0.45^Ref			Pulsation ephemeris	Max (V) = 2455150 + 284.2 x E^Ref

Hot component

Type/Spectral type	WD^Ref	Mass (M_⊙)	0.6^Ref	Spin period (min)	-
Shell-burning/Accreting-only	shell-burning^Ref	Radius (R_⊙)	0.06^Ref	Accretion disk	-
Eff. temperature (K)	55000-70000^Ref, 158000^Ref	Luminosity (L_⊙)	2000^Ref
Lower limit (K)	-
Upper limit (K)	-

Links

SIMBAD CDS Portal

Notes

Initially classified as a PN, observations by Allen (1974) noted that the spectrum resembles a late-type star, suggesting a possible symbiotic nature (Bond, 1976). It was later confirmed as a symbiotic star by Kondrateva (1992). Subsequent analysis confirmed that the cool component is a dust-free Mira variable, as reported in Munari et al. (2010).

References

Allen, D. A., 1974, MNRAS, 168, 1, 1974MNRAS.168....1A
Bond, H. E., 1976, PASP, 88, 192, 1976PASP...88..192B
Kondrateva, L. N., 1992, SvA, 36, 624, 1992SvA....36..624K
Kondratyeva, L. N., Denissyuk, E. K., 2008, A&A, 479, 2, 529, 2008A&A...479..529K
Munari, U., Siviero, A., Dallaporta, S. et al., 2010, MNRAS, 407, 2, 1070, 2010MNRAS.407.1070M

LL Cas