Star in the constellation Columba
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! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000.0
      Equinox J2000.0 (ICRS)
! style="text-align:left" | Constellation
! style="text-align:left" | Right ascension
! style="text-align:left" | Declination
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:left" | Spectral type
! style="text-align:left" | U−B 
! style="text-align:left" | B−V 
! style="text-align:left" | R−I 
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Alpha Columbae or α Columbae, officially named Phact (), is a third magnitude star in the southern constellation of Columba. It has an apparent visual magnitude of 2.6, making it the brightest member of Columba. Based upon parallax measurements made during the Hipparcos mission, Alpha Columbae is located at a distance of around .
Nomenclature.
"α Columbae", Latinized to "Alpha Columbae", is the star's Bayer designation.
The traditional name of "Phact" (also rendered "Phad", "Phaet", "Phakt") derives from the Arabic فاختة "fākhitah" 'ring dove'. It was originally applied to the constellation Cygnus and later transferred to this star. The etymology of its name "hadāri" (unknown meaning) has also been suggested. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included "Phact" for this star.
In Chinese, (), meaning "Grandfather", refers to an asterism consisting of α Columbae and ε Columbae. Consequently, α Columbae itself is known as (, .). From this Chinese name, the name "Chang Jin" has appeared
Properties.
This is believed to be a solitary star, although it has a faint optical companion at an angular separation of 13.5 arcseconds, making it a double star. The stellar classification of Alpha Columbae is B9Ve, matching a B-type main-sequence star. The spectrum shows it to be a Be star surrounded by a hot gaseous disk, which is generating emission lines because of hydrogen recombination. Like most if not all such stars, it is rotating rapidly with a projected rotational velocity of 176 km s−1. The azimuthal equatorial velocity may be 457 km s−1. It is a suspected Gamma Cassiopeiae type (GCAS) variable star, with its apparent magnitude varying from 2.62m to 2.66m.
References.
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