Star in the constellation Ara
! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000.0      Equinox J2000.0
! 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" | B−V 
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HD 154672 is a yellow subgiant (spectral type G3 IV). It is about 65 parsecs away from the Sun that is larger than, but of a similar mass to, the Sun. However, HD 154672 is much older. The star is very metal-rich, which is one of the reasons why it was targeted for a planet search by the N2K Consortium, which discovered the gas giant planet HD 154672 b using Doppler Spectroscopy; the discovery was reported in October 2008. The N2K collaboration chose HD 154672 primarily because it aimed to discover the correlation between a star's metallicity and the mass of orbiting planets.
HD 154672 was targeted by the Magellan Telescopes. It is the host of the first planet discovered from the telescopes by N2K.
Observational history.
HD 154672 was first targeted for a planet search in 2004 by the N2K Consortium, a collaboration of astronomers hoping to take radial velocity measurements of previously untargeted stars using Doppler spectroscopy; however, HD 154672 had been previously targeted by a series of surveys, and was previously included in the Henry Draper catalog and the catalog of the European Space Agency's Hipparcos satellite.
N2K deliberately biased its search towards closely orbiting Jupiter-size planets (Hot Jupiters) in the orbit of metal-rich stars, as the consortium hoped to discover how the mass of a planet relates to its host star's metal content. Initially, HD 154672 was noted as a host to a short-orbit Hot Jupiter, although additional observations revealed that the prospective planetary body had a longer orbit than previously expected, as revealed by the Magellan Telescopes at Chile's Las Campanas Observatory.
Use of the Magellan Clay telescope's Magellan Inamori Kyocera Echelle spectrograph (MIKE) helped collect sixteen radial velocity measurements for HD 154672; a team of American astronomers and one from the Vatican City used these measurements to confirm the existence of planet HD 154672 b and to determine its mass.
The discovery of HD 154672's planet was reported in the "Astronomical Journal" on October 7, 2008 along with a planet in the orbit of HD 205739.
Host star.
HD 154672 is a sunlike G-type star that has a mass of 1.06 times that of the Sun and a radius that is 1.27 times that of the Sun. Thus, it is slightly larger than the Sun, although it has a similar mass. The star has an effective temperature of 5714 K, slightly cooler than the Sun; however, it is far richer in iron, with a measured metallicity of [Fe/H] = 0.26. This means that the star has 1.82 times more iron than the Sun does. HD 154672 is far older than the Sun, as its estimated gyrochronological age is estimated at 9.28 billion years. HD 154672's spectrum suggests that the star's chromosphere (its outer layer) is not active.
HD 154672 is located 65.8 parsecs (214.6 light years) away from Earth. It has an apparent magnitude (V) of 8.22, making the star too dim to see from Earth with the naked eye. The star is slightly dimmer than planet Neptune as perceived with the naked eye, which has an apparent magnitude of 7.78 at its brightest. The star's actual brightness is measured with an absolute magnitude of 4.12, similar to that of the Sun.
Planetary system.
HD 154672 b is a Hot Jupiter, as it is a closely orbiting planet with a high mass. Specifically, HD 154672 has a mass that is 5.02 times greater than Jupiter's mass. It also orbits at a distance of 0.6 AU, or about 60% of the mean distance between the Earth and Sun. This orbit is completed every 163.91 days.
HD 154672 b has an orbital eccentricity of 0.61, denoting a very elliptical orbit. The planet's discoverers noted that if water existed in the planet's atmosphere, it might change from a liquid state to a gaseous state as the planet swings closer to its host star, increasing its temperature.
! align=center| Companion
! align=center| Mass
! align=center| Semimajor axis
! align=center| Orbital period
! align=center| Eccentricity
! align=center| Inclination
! align=center| Radius
References.
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 ;indicator name="01-sky-coordinates" ; ;templatestyles src="Template:Sky/styles.css" / ;Coordinates: &amp;show_grid=1&amp;show_constellation_lines=1&amp;show_constellation_boundaries=1&amp;show_const_names=1&amp;show_galaxies=1&amp;img_source=IMG_all 17h 10m 04.9121s, −56° 26′ 57.364″ ;/indicator ;