M31N 2022-09b
POSSIBLE
M31
Constellation
Andromeda |
Equatorial coordinates
α = 00 42 37.880
δ = +41 12 49.100 |
Galactic coordinates
l = 121.1504°
b = -21.6276° |
| Suspected |
2022Ref |
| Confirmed |
- |
| Symbiotic IR type |
- |
| Hot component type |
accreting-only?Ref |
| Outbursts |
YesRef - SyN?Ref |
|
|
Identifiers
| M31N 2022-09b |
IRAS - |
GSC2.4.2 NBVE283898 |
AAVSO - |
| SIMBAD - |
Pan-STARRS - |
SAO - |
VSX - |
| GAIA DR3 - |
SkyMapper - |
WRAY - |
GCVS - |
| 2MASS - |
HIP - |
Hen - |
BD - |
| WISE - |
TYC - |
ESO - |
HD - |
Symbiotic Catalogs
| Bidelman (1954) |
- |
Allen (1984) |
- |
Belzcyński et al. (2001) |
- |
| Gaposchkin (1957) |
- |
Kenyon (1986) |
- |
Akras et al. (2019) |
- |
| Boyarchuk (1969) |
- |
Vaidis (1988, 1991) |
- |
Position
| Right ascension (°) |
10.6578Ref |
Parallax (mas) |
- |
Reddening E(B-V) (mag) |
0.39±0.11Ref, Note |
| Declination (°) |
41.2136Ref |
Distance (kpc) |
785±25Ref
-, Note |
|
|
| Galactic longitude (°) |
121.1504Ref |
Proper motion in α (mas/yr) |
- |
|
|
| Galactic latitude (°) |
-21.6276Ref |
Proper motion in δ (mas/yr) |
- |
|
|
Observations
| X-Ray |
- |
IR type |
- |
Radio |
- |
| X-Ray type |
- |
J (mag) |
- |
Flickering |
- |
| GALEX FUV (mag) |
- |
H (mag) |
- |
Outbursts |
YesRef |
| GALEX NUV (mag) |
- |
K (mag) |
- |
Outburst type |
SyN?Ref |
| IUE |
NoRef |
WISE W1 (mag) |
- |
Jets |
- |
| FUSE |
NoRef |
WISE W2 (mag) |
- |
Resolved nebula |
- |
| U (mag) |
- |
WISE W3 (mag) |
- |
IPmax (eV) |
- |
| B (mag) |
- |
WISE W4 (mag) |
- |
[O III] lines |
- |
| V (mag) |
- |
IRAS 12μm (Jy) |
- |
He II lines |
- |
| R (mag) |
- |
IRAS 25μm (Jy) |
- |
[Fe VII] lines |
- |
| I (mag) |
- |
IRAS 60μm (Jy) |
- |
O VI lines |
- |
| BP (mag) |
- |
IRAS 100μm (Jy) |
- |
|
|
| G (mag) |
- |
AKARI S09 (Jy) |
- |
|
|
| RP (mag) |
- |
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 |
- |
| Orbital ephemeris |
- |
|
|
|
|
Cool component
| Spectral type |
- |
Mass (M⊙) |
- |
Pulsation |
- |
| Eff. temperature (K) |
- |
Radius (R⊙) |
- |
Type |
- |
| IR type |
- |
Luminosity (L⊙) |
- |
Pulsation period (days) |
- |
| Metallicity [Fe/H] |
- |
|
|
Pulsation ephemeris |
- |
Hot component
| Type/Spectral type |
- |
Mass (M⊙) |
- |
Spin period (min) |
- |
| Shell-burning/Accreting-only |
accreting-only?Ref |
Radius (R⊙) |
- |
Accretion disk |
- |
| Eff. temperature (K) |
- |
Luminosity (L⊙) |
- |
|
|
| Lower limit (K) |
- |
|
|
|
|
| Upper limit (K) |
- |
|
|
|
|
Notes
Detected in a slow nova-like outburst as reported in Zhang et al. (2022) and Hornoch et al. (2022), the authors claimed that the object exhibited Hα excess after the brightness maximum, thus ruling out Mira variability. Symbiotic nature was suggested by Róbert Fidrich on the Transient Name Server (https://www.wis-tns.org/object/2022abzg) based on the blue colors observed at maximum brightness.
References
- Hornoch, K., Kucakova, H., Shafter, A. W. et al., 2022, ATel, 15831, 1, 2022ATel15831....1H
- Zhang, M., Tang, L., Zhao, J. et al., 2022, TNSTR, 2022-3483, 1, 2022TNSTR3483....1Z
Last updated: December 31, 2022