![]() HD 168625 is the left star of the pair below the Omega Nebula. The other is the hypergiant HD 168607. | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Sagittarius |
Right ascension | 18h 21m 19.548s [1] |
Declination | −16° 22′ 16.0572″ [1] |
Apparent magnitude (V) | 8.30–8.41 [2] |
Characteristics | |
Spectral type | B6Ia+ [3] (B2—B8 [4]) May be B60 due to hypergiant designation |
U−B color index | +0.37 [5] |
B−V color index | +1.41 [5] |
J−K color index | 0.599 |
Variable type | α Cygni [6] |
Astrometry | |
Radial velocity (Rv) | −4.00 [7] km/s |
Proper motion (μ) |
RA: −0.71±1.20
[1]
mas/
yr Dec.: +0.01±0.74 [1] mas/ yr |
Parallax (π) | 0.6212 ± 0.0640 mas [8] |
Distance | approx. 5,300
ly (approx. 1,600 pc) |
Absolute magnitude (MV) | −8.39 [4] |
Details [4] | |
Radius | 105 R☉ |
Luminosity | 380,000 L☉ |
Surface gravity (log g) | 1.74 cgs |
Temperature | 14,000 K |
Rotational velocity (v sin i) | 60 km/s |
Other designations | |
Database references | |
SIMBAD | data |
HD 168625 (V4030 Sagittarii) is a blue hypergiant star and candidate luminous blue variable located in the constellation of Sagittarius easy to see with amateur telescopes. It forms a visual pair with the also blue hypergiant (and luminous blue variable) HD 168607 and is located to the south-east of M17, the Omega Nebula.
The distance of HD 168625 and its association with the Omega Nebula and HD 168607 is in doubt; while some authors think both stars are physically associated and belong to the stellar association Serpens OB1, [9] at a distance to the Sun of 2.2 kiloparsecs (7,200 ly), [10] or for both per Gaia Data Release 2 about 1.6 kiloparsecs (5,200 ly), [8] a 2002 study estimates this star is farther, at about 2.8 kiloparsecs (9,100 ly) and unrelated to the other two objects. [11]
Assuming a distance of 2.2 kiloparsecs, the star would be 220,000 times brighter than the Sun, having a surface temperature of 12,000 K. [10] At that distance it can be calculated to be losing mass through a fierce stellar wind at roughly 1.46×10−6 solar masses per year [13] however this is to be muted somewhat as work realized in 2012 from the VLT reveal a binary star system – [14] a companion exists around 4.5 magnitudes fainter than the primary. [15]
The most notable characteristic of HD 168625 is the presence of a nebula surrounding it that was discovered in 1994 [16] and that has been studied with the help of several instruments and observatories and telescopes that include among others the Hubble Space Telescope [11] and the VLT. [13]
Said studies show that HD 168625 is actually surrounded by two nebulae: an inner one that has an elliptical shape and a very complex structure that includes arcs and filaments, [11] and a much larger outer one discovered with the help of the Spitzer Space Telescope that has a bipolar shape and that looks like a clone of the one surrounding Sanduleak -69° 202, the progenitor of the supernova 1987A in the Large Magellanic Cloud. [17] This suggests Sanduleak −69° 202 was also a luminous blue variable as well as the possibility of HD 168625 exploding as a Type II supernova in the near future. [17]
East-north-east of the star and nebula is HD 168701 (HIP 90001), an eclipsing binary of beta Lyrae type. [18] It is at about six times the angular separation of HD 168607 viewed from the solar system and is the third very bright point to the south-east of the nebula. Its parallax of 0.7106 ± 0.0451 mas implies it is about 1,700 parsecs (5,500 ly) away. [18]
![]() HD 168625 is the left star of the pair below the Omega Nebula. The other is the hypergiant HD 168607. | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Sagittarius |
Right ascension | 18h 21m 19.548s [1] |
Declination | −16° 22′ 16.0572″ [1] |
Apparent magnitude (V) | 8.30–8.41 [2] |
Characteristics | |
Spectral type | B6Ia+ [3] (B2—B8 [4]) May be B60 due to hypergiant designation |
U−B color index | +0.37 [5] |
B−V color index | +1.41 [5] |
J−K color index | 0.599 |
Variable type | α Cygni [6] |
Astrometry | |
Radial velocity (Rv) | −4.00 [7] km/s |
Proper motion (μ) |
RA: −0.71±1.20
[1]
mas/
yr Dec.: +0.01±0.74 [1] mas/ yr |
Parallax (π) | 0.6212 ± 0.0640 mas [8] |
Distance | approx. 5,300
ly (approx. 1,600 pc) |
Absolute magnitude (MV) | −8.39 [4] |
Details [4] | |
Radius | 105 R☉ |
Luminosity | 380,000 L☉ |
Surface gravity (log g) | 1.74 cgs |
Temperature | 14,000 K |
Rotational velocity (v sin i) | 60 km/s |
Other designations | |
Database references | |
SIMBAD | data |
HD 168625 (V4030 Sagittarii) is a blue hypergiant star and candidate luminous blue variable located in the constellation of Sagittarius easy to see with amateur telescopes. It forms a visual pair with the also blue hypergiant (and luminous blue variable) HD 168607 and is located to the south-east of M17, the Omega Nebula.
The distance of HD 168625 and its association with the Omega Nebula and HD 168607 is in doubt; while some authors think both stars are physically associated and belong to the stellar association Serpens OB1, [9] at a distance to the Sun of 2.2 kiloparsecs (7,200 ly), [10] or for both per Gaia Data Release 2 about 1.6 kiloparsecs (5,200 ly), [8] a 2002 study estimates this star is farther, at about 2.8 kiloparsecs (9,100 ly) and unrelated to the other two objects. [11]
Assuming a distance of 2.2 kiloparsecs, the star would be 220,000 times brighter than the Sun, having a surface temperature of 12,000 K. [10] At that distance it can be calculated to be losing mass through a fierce stellar wind at roughly 1.46×10−6 solar masses per year [13] however this is to be muted somewhat as work realized in 2012 from the VLT reveal a binary star system – [14] a companion exists around 4.5 magnitudes fainter than the primary. [15]
The most notable characteristic of HD 168625 is the presence of a nebula surrounding it that was discovered in 1994 [16] and that has been studied with the help of several instruments and observatories and telescopes that include among others the Hubble Space Telescope [11] and the VLT. [13]
Said studies show that HD 168625 is actually surrounded by two nebulae: an inner one that has an elliptical shape and a very complex structure that includes arcs and filaments, [11] and a much larger outer one discovered with the help of the Spitzer Space Telescope that has a bipolar shape and that looks like a clone of the one surrounding Sanduleak -69° 202, the progenitor of the supernova 1987A in the Large Magellanic Cloud. [17] This suggests Sanduleak −69° 202 was also a luminous blue variable as well as the possibility of HD 168625 exploding as a Type II supernova in the near future. [17]
East-north-east of the star and nebula is HD 168701 (HIP 90001), an eclipsing binary of beta Lyrae type. [18] It is at about six times the angular separation of HD 168607 viewed from the solar system and is the third very bright point to the south-east of the nebula. Its parallax of 0.7106 ± 0.0451 mas implies it is about 1,700 parsecs (5,500 ly) away. [18]