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{{Short description|Exoplanet}}
{{Short description|Young exoplanet orbiting the red dwarf TOI-1227}}
{{Sky|12|27|04.31|-|72|27|06.49}}
{{Sky|12|27|04.31|-|72|27|06.49}}
{{Infobox planet
{{Infobox planet
| caption =
| apsis = astron
| apsis = astron
| discoverer = [[TESS Hunt for Young and Maturing Exoplanets|THYME]] (Mann et al.)
| discoverer = Mann et al. ([[TESS Hunt for Young and Maturing Exoplanets|THYME]])
| discovery_site =
| periastron =
| apoastron =
| period =
| synodic_period =
| mean_radius = {{val|0.854|0.067|0.052}} {{Jupiter radius|link=true}}
| mean_radius = {{val|0.854|0.067|0.052}} {{Jupiter radius|link=true}}
| density =
| moment_of_inertia_factor =
| escape_velocity =
| name = TOI-1227 b
| name = TOI-1227 b
| image =
| image_size =
| image_alt =
| discovered = 2022
| discovered = 2022
| discovery_method = [[Transit (astronomy)|Transit Method]]
| discovery_method = [[Transit (astronomy)|Transit method]]
| discovery_ref = <ref name="Mann et al" />
| discovery_ref = <ref name="Mann et al" />
| alt_names =
| extrasolarplanet = yes
| extrasolarplanet = yes
| semimajor = {{val|0.0886|0.0054|0.0057|u=au}}
| semimajor = {{val|0.0886|0.0054|0.0057|u=AU}}
| eccentricity =
| avg_speed =
| inclination = {{val|88.571|0.062|0.093}} °
| inclination = {{val|88.571|0.062|0.093}} °
⚫
| star = TOI-1227 (Gaia DR2 5842480953772012928)
| angular_dist =
| long_periastron =
| time_periastron =
| arg_peri =
| semi-amplitude =
⚫
| star = [[Gaia DR2 5842480953772012928]]
| orbit_ref =
| volume =
| mass =
| surface_grav =
| albedo =
| single_temperature =
| physical_ref =
}}
}}


'''TOI-1227 b''' is one of the youngest transiting [[exoplanet]]s discovered (as of September 2022). The others are [[K2-33b]] and [[HIP 67522 b]]. The exoplanet TOI-1227 b is about 11±2 Myrs old and currently {{Earth radius|9.5|link=true}} large. It will become a {{Earth radius|3-5}} planet in about 1&nbsp;billion years, because the planet is still contracting. TOI-1227 b orbits a very low-mass star every 27.36 days.<ref name="Mann et al">{{Cite journal |last1=Mann |first1=Andrew W. |last2=Wood |first2=Mackenna L. |last3=Schmidt |first3=Stephen P. |last4=Barber |first4=Madyson G. |last5=Owen |first5=James E. |last6=Tofflemire |first6=Benjamin M. |last7=Newton |first7=Elisabeth R. |last8=Mamajek |first8=Eric E. |last9=Bush |first9=Jonathan L. |last10=Mace |first10=Gregory N. |last11=Kraus |first11=Adam L. |last12=Thao |first12=Pa Chia |last13=Vanderburg |first13=Andrew |last14=Llama |first14=Joe |last15=Johns-Krull |first15=Christopher M. |date=2022-04-01 |title=TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux |url=https://ui.adsabs.harvard.edu/abs/2022AJ....163..156M |journal=The Astronomical Journal |volume=163 |issue=4 |pages=156 |doi=10.3847/1538-3881/ac511d |arxiv=2110.09531 |bibcode=2022AJ....163..156M |s2cid=239024522 |issn=0004-6256}}</ref>
'''TOI-1227 b''' is one of the youngest transiting [[exoplanet]]s discovered (as of September 2022), alongside [[K2-33b]] and [[HIP 67522 b]]. The exoplanet TOI-1227 b is about {{val|11|2}} million years old{{Efn|For comparison, the Solar System is about 4.6 billion years old.}} and currently {{Earth radius|9.6|link=true}} large. It will become a {{Earth radius|3-5}} planet in about 1&nbsp;billion years, because the planet is still contracting. TOI-1227 b orbits its host star every 27.36 days.<ref name="Mann et al">{{Cite journal |last1=Mann |first1=Andrew W. |last2=Wood |first2=Mackenna L. |last3=Schmidt |first3=Stephen P. |last4=Barber |first4=Madyson G. |last5=Owen |first5=James E. |last6=Tofflemire |first6=Benjamin M. |last7=Newton |first7=Elisabeth R. |last8=Mamajek |first8=Eric E. |last9=Bush |first9=Jonathan L. |last10=Mace |first10=Gregory N. |last11=Kraus |first11=Adam L. |last12=Thao |first12=Pa Chia |last13=Vanderburg |first13=Andrew |last14=Llama |first14=Joe |last15=Johns-Krull |first15=Christopher M. |date=2022-04-01 |title=TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux |journal=The Astronomical Journal |volume=163 |issue=4 |pages=156 |doi=10.3847/1538-3881/ac511d |arxiv=2110.09531 |bibcode=2022AJ....163..156M |s2cid=239024522 |issn=0004-6256 |doi-access=free }}</ref>


== Characteristics ==
== Characteristics ==
TOI-1227 b has a size that is 85% that of [[Jupiter]]. No other Jupiter-sized planet was detected around mid- to late [[Red dwarf|M-dwarfs]], despite the deep transits such a planet would create. The researchers find that the planet is still hot from its formation and this heat, combined with a hydrogen-dominated [[primary atmosphere]] makes the atmosphere of TOI-1227 b inflated. Evolutionary models suggest that TOI-1227 b will eventually evolve into a [[sub-Neptune]] within the next billion years.<ref name="Mann et al" />
TOI-1227 b has a size that is 85% that of [[Jupiter]], or 9.6 times that of Earth. No other Jupiter-sized planet was detected around mid- to late [[Red dwarf|M-dwarfs]], despite the deep transits such a planet would create. The researchers find that the planet is still hot from its formation and this heat, combined with a hydrogen-dominated [[primary atmosphere]] makes the atmosphere of TOI-1227 b inflated. Evolutionary models suggest that TOI-1227 b will eventually evolve into a [[sub-Neptune]] within the next billion years.<ref name="Mann et al" />


=== Future research ===
=== Future research ===
[[Radial velocity]] follow-up to determine the [[mass]] of TOI-1227 b is not possible in the [[Visible-light astronomy|optical]], but might be possible in the [[Infrared|near-infrared]]. A less challenging follow-up would be the measurement of the Spin-Orbit-Alignment via the [[Rossiter–McLaughlin effect|Rossiter-McLaughlin effect]].<ref name="Mann et al" />
[[Radial velocity]] follow-up to determine the [[mass]] of TOI-1227 b is not possible in the [[Visible-light astronomy|optical]], but might be possible in the [[Infrared|near-infrared]]. A less challenging follow-up would be the measurement of the Spin-Orbit-Alignment via the [[Rossiter–McLaughlin effect]].<ref name="Mann et al" />


== Host star ==
== Host star ==
{{Starbox begin|name=TOI-1227}}
TOI-1227 is located north of the globular cluster [[NGC 4372]], but it is much closer to earth than this cluster of stars at a distance of about 101 [[parsec]].<ref name="Mann et al" />
{{Starbox observe
|epoch=J2000
|constell=[[Musca]]{{Efn|Obtained with a right ascension of {{RA|12|27|4.31}} and a declination of {{DEC|-72|27|6.5}}<ref name="SIMBAD"/> on this [https://djm.cc/constellation.html website].|name=Constellation|group=note}}
|equinox=J2000
|ra={{RA|12|27|4.31}}<ref name="SIMBAD"/>
|dec={{DEC|-72|27|6.5}}<ref name="SIMBAD"/>
|appmag_v=17{{±|1.133}}<ref name="NASA">{{Cite web |title=TOI-1227 {{!}} NASA Exoplanet Archive |url=https://exoplanetarchive.ipac.caltech.edu/overview/TOI-1227 |access-date=2024-02-14 |website=exoplanetarchive.ipac.caltech.edu}}</ref>
}}
{{Starbox character
|type=[[Pre-main sequence star]]<ref name="Mann et al"/>
|class=M4.5V-M5V<ref name="Mann et al"/>
}}
{{Starbox astrometry
|radial_v={{Val|13.3|0.3}}<ref name="Mann et al"/>
|prop_mo_ra={{Val|-40.2658|0.0972}}
|pm_footnote=<ref name="NASA"/>
|prop_mo_dec={{Val|-10.6417|0.0807}}
|parallax=9.9079
|p_error=0.0558
|parallax_footnote=<ref name="NASA"/>
|dist_ly={{Val|328.089|1.87|1.845}}
|dist_footnote=<ref name="NASA"/>
|dist_pc={{Val|100.641|0.573|0.566}}
|absmag_v=11.986{{Efn|1=Calculated using an [[apparent magnitude]] of 17 and a distance of 100.641 [[parsec]]s<ref name="NASA"/> in the equation M{{sub|app}} = M{{sub|abs}} - 5 + 5 * log(distance (parsecs))}}
}}
{{Starbox detail
|mass={{Val|0.17|0.015}}
|radius={{Val|0.56|0.03}}
|luminosity=0.0251
|gravity={{Val|4.7893|0.0058}}<ref name="NASA"/>
|temperature={{Val|3072|74}}
|rotation={{Val|1.65|0.04|ul=day}}
|rotational_velocity={{Val|16.65|0.24}}
|age_myr={{Val|11|2}}
|source=<ref name="Mann et al"/>
}}
{{Starbox catalog
|names=2MASS J12270432-7227064, [[Gaia DR2]], 5842480953772012928, [[Gaia DR3]] 5842480953772012928, [[TESS Input Catalog|TIC]] 360156606, [[Tess Object of Interest|TOI]]-1227, [[UCAC4]] 088-032065, [[Wide-field Infrared Survey Explorer|WISE]] J122704.24-722706.5, [[Wide-field Infrared Survey Explorer|WISEA]] J122704.22-722706.5<ref name="SIMBAD"/>}}
{{Starbox end}}
⚫
TOI-1227 was first identified as a [[pre-main-sequence star]] (PMS star) with the [[Gaia (spacecraft)|Gaia satellite]].<ref name="harvard">{{Cite journal |last1=Goldman |first1=Bertrand |last2=Röser |first2=Siegfried |last3=Schilbach |first3=Elena |last4=Moór |first4=Attila C. |last5=Henning |first5=Thomas |date=2018-11-01 |title=A Large Moving Group within the Lower Centaurus Crux Association |journal=The Astrophysical Journal |volume=868 |issue=1 |pages=32 |doi=10.3847/1538-4357/aae64c |arxiv=1807.02076 |bibcode=2018ApJ...868...32G |s2cid=119343278 |issn=0004-637X |doi-access=free }}</ref><ref>{{Cite journal |last1=Zari |first1=E. |last2=Hashemi |first2=H. |last3=Brown |first3=A. G. A. |last4=Jardine |first4=K. |last5=de Zeeuw |first5=P. T. |date=2018-12-01 |title=3D mapping of young stars in the solar neighbourhood with Gaia DR2 |url=https://ui.adsabs.harvard.edu/abs/2018A&A...620A.172Z |journal=Astronomy and Astrophysics |volume=620 |pages=A172 |doi=10.1051/0004-6361/201834150 |arxiv=1810.09819 |bibcode=2018A&A...620A.172Z |s2cid=119078481 |issn=0004-6361}}</ref><ref name="Kerr 23">{{Cite journal |last1=Kerr |first1=Ronan M. P. |last2=Rizzuto |first2=Aaron C. |last3=Kraus |first3=Adam L. |last4=Offner |first4=Stella S. R. |date=2021-08-01 |title=Stars with Photometrically Young Gaia Luminosities Around the Solar System (SPYGLASS). I. Mapping Young Stellar Structures and Their Star Formation Histories |journal=The Astrophysical Journal |volume=917 |issue=1 |pages=23 |doi=10.3847/1538-4357/ac0251 |arxiv=2105.09338 |bibcode=2021ApJ...917...23K |s2cid=234790391 |issn=0004-637X |doi-access=free }}</ref> Without this prior identification as a PMS star the exoplanet signal of TOI-1227 b would have been disregarded as an [[eclipsing binary]] due to the V-shape of the transit signal.<ref name="Mann et al" />


The star is located north of the globular cluster [[NGC 4372]], but it is much closer to earth than this cluster of stars, at a distance of about {{convert|101|pc|ly|lk=on|abbr=off}}.<ref name="Mann et al" /> NGC 4372 is {{convert|5800|pc|ly}} away.<ref>{{Cite journal |last=Boyles |first=Jason |last2=Lorimer |first2=Duncan R. |last3=Turk |first3=Phil J. |last4=Mnatsakanov |first4=Robert |last5=Lynch |first5=Ryan S. |last6=Ransom |first6=Scott M. |last7=Freire |first7=Paulo C. |last8=Belczynski |first8=Khris |date=2011-11-20 |title=Young Radio Pulsars in Galactic Globular Clusters |url=http://arxiv.org/abs/1108.4402 |journal=The Astrophysical Journal |volume=742 |issue=1 |pages=51 |doi=10.1088/0004-637X/742/1/51 |issn=0004-637X|arxiv=1108.4402 }}</ref>
⚫
TOI-1227 was first identified as a [[pre-main-sequence star]] (PMS star) with the [[Gaia (spacecraft)|Gaia satellite]].<ref name="harvard">{{Cite journal |last1=Goldman |first1=Bertrand |last2=Röser |first2=Siegfried |last3=Schilbach |first3=Elena |last4=Moór |first4=Attila C. |last5=Henning |first5=Thomas |date=2018-11-01 |title=A Large Moving Group within the Lower Centaurus Crux Association |url=https://ui.adsabs.harvard.edu/abs/2018ApJ...868...32G |journal=The Astrophysical Journal |volume=868 |issue=1 |pages=32 |doi=10.3847/1538-4357/aae64c |arxiv=1807.02076 |bibcode=2018ApJ...868...32G |s2cid=119343278 |issn=0004-637X}}</ref><ref>{{Cite journal |last1=Zari |first1=E. |last2=Hashemi |first2=H. |last3=Brown |first3=A. G. A. |last4=Jardine |first4=K. |last5=de Zeeuw |first5=P. T. |date=2018-12-01 |title=3D mapping of young stars in the solar neighbourhood with Gaia DR2 |url=https://ui.adsabs.harvard.edu/abs/2018A&A...620A.172Z |journal=Astronomy and Astrophysics |volume=620 |pages=A172 |doi=10.1051/0004-6361/201834150 |arxiv=1810.09819 |bibcode=2018A&A...620A.172Z |s2cid=119078481 |issn=0004-6361}}</ref><ref name="Kerr 23">{{Cite journal |last1=Kerr |first1=Ronan M. P. |last2=Rizzuto |first2=Aaron C. |last3=Kraus |first3=Adam L. |last4=Offner |first4=Stella S. R. |date=2021-08-01 |title=Stars with Photometrically Young Gaia Luminosities Around the Solar System (SPYGLASS). I. Mapping Young Stellar Structures and Their Star Formation Histories |url=https://ui.adsabs.harvard.edu/abs/2021ApJ...917...23K |journal=The Astrophysical Journal |volume=917 |issue=1 |pages=23 |doi=10.3847/1538-4357/ac0251 |arxiv=2105.09338 |bibcode=2021ApJ...917...23K |s2cid=234790391 |issn=0004-637X}}</ref> Without this prior identification as a PMS star the exoplanet signal of TOI-1227 b would have been disregarded as an [[eclipsing binary]] due to the V-shape of the transit signal.<ref name="Mann et al" />


The host star TOI-1227 is part of a subgroup of the [[Scorpius–Centaurus association|Lower Centaurus Crux]] OB association, sometimes called B,<ref name="Kerr 23"/> A0<ref name="harvard"/> and called Musca group by the scientists that discovered TOI-1227 b. This group was called Musca after the constellation [[Musca]] in which most of its members are located.<ref name="Mann et al" />
The host star TOI-1227 is part of a subgroup of the [[Scorpius–Centaurus association|Lower Centaurus Crux]] OB association, sometimes called B,<ref name="Kerr 23"/> A0<ref name="harvard"/> and called Musca group by the scientists that discovered TOI-1227 b. This group was called Musca after the constellation [[Musca]] in which most of its members are located.<ref name="Mann et al" />


TOI-1227 has a spectral type of M4.5V to M5V, a mass 17% of the [[sun]] and a radius 56% of the sun. The host star is relative faint for a TOI with a V-band magnitude of about 17. The host star shows [[Lithium]] in its atmosphere, which should be depleted within 10-200 Myrs for M-dwarfs.<ref name="Mann et al" />
TOI-1227 has a spectral type of M4.5V to M5V, a mass 17% of the [[Sun]] and a radius 56% of the Sun. The host star is relative faint for a TOI with a [[visual magnitude]] of about 17.<ref name="Mann et al" /> The right ascension of {{RA|12|27|4.31}} and the declination {{DEC|-72|27|6.5}} implies that it is located in the Musca constellation.<ref name="SIMBAD">{{Cite web |title=TOI-1227|url=https://simbad.cds.unistra.fr/mobile/object.html?object_name=TOI-1227 |access-date=2024-02-14 |website=simbad.cds.unistra.fr}}</ref>{{Efn|The constellation can be obtained by the right ascension and declination in this [https://djm.cc/constellation.html website].}} The host star shows [[Lithium]] in its atmosphere, which should be depleted within 10-200 million years for M-dwarfs.<ref name="Mann et al" />


== References ==
== References ==
{{reflist}}
{{reflist}}

{{2022 in space}}
{{2022 in space}}


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[[Category:Exoplanets discovered in 2022]]
[[Category:Exoplanets discovered in 2022]]
[[Category:Protoplanets]]
[[Category:Protoplanets]]
<references group="lower-alpha" />
<references group="note" />

Latest revision as of 15:51, 23 February 2024

TOI-1227 b
Discovery[1]
Discovered byMann et al. (THYME)
Discovery date2022
Transit method
Orbital characteristics
0.0886+0.0054
−0.0057 AU
Inclination88.571+0.062
−0.093 °
StarTOI-1227 (Gaia DR2 5842480953772012928)
Physical characteristics
0.854+0.067
−0.052 RJ

TOI-1227 b is one of the youngest transiting exoplanets discovered (as of September 2022), alongside K2-33b and HIP 67522 b. The exoplanet TOI-1227 b is about 11±2 million years old[a] and currently 9.6 R🜨 large. It will become a 3-5 R🜨 planet in about 1 billion years, because the planet is still contracting. TOI-1227 b orbits its host star every 27.36 days.[1]

Characteristics

[edit]

TOI-1227 b has a size that is 85% that of Jupiter, or 9.6 times that of Earth. No other Jupiter-sized planet was detected around mid- to late M-dwarfs, despite the deep transits such a planet would create. The researchers find that the planet is still hot from its formation and this heat, combined with a hydrogen-dominated primary atmosphere makes the atmosphere of TOI-1227 b inflated. Evolutionary models suggest that TOI-1227 b will eventually evolve into a sub-Neptune within the next billion years.[1]

Future research

[edit]

Radial velocity follow-up to determine the mass of TOI-1227 b is not possible in the optical, but might be possible in the near-infrared. A less challenging follow-up would be the measurement of the Spin-Orbit-Alignment via the Rossiter–McLaughlin effect.[1]

Host star

[edit]
TOI-1227
Observation data
Epoch J2000      Equinox J2000
Constellation Musca[note 1]
Right ascension 12h 27m 4.31s[2]
Declination −72° 27′ 6.5″[2]
Apparent magnitude (V) 17±1.133[3]
Characteristics
Evolutionary stage Pre-main sequence star[1]
Spectral type M4.5V-M5V[1]
Astrometry
Radial velocity (Rv)13.3±0.3[1] km/s
Proper motion (μ) RA: −40.2658±0.0972 mas/yr[3]
Dec.: −10.6417±0.0807 mas/yr[3]
Parallax (π)9.9079 ± 0.0558 mas[3]
Distance328.089+1.87
−1.845 ly
(100.641+0.573
−0.566 pc)[3]
Absolute magnitude (MV)11.986[b]
Details[1]
Mass0.17±0.015 M☉
Radius0.56±0.03 R☉
Luminosity0.0251 L☉
Surface gravity (log g)4.7893±0.0058[3] cgs
Temperature3072±74 K
Rotation1.65±0.04 d
Rotational velocity (v sin i)16.65±0.24 km/s
Age11±2 Myr
Other designations
2MASS J12270432-7227064, Gaia DR2, 5842480953772012928, Gaia DR3 5842480953772012928, TIC 360156606, TOI-1227, UCAC4 088-032065, WISE J122704.24-722706.5, WISEA J122704.22-722706.5[2]

TOI-1227 was first identified as a pre-main-sequence star (PMS star) with the Gaia satellite.[4][5][6] Without this prior identification as a PMS star the exoplanet signal of TOI-1227 b would have been disregarded as an eclipsing binary due to the V-shape of the transit signal.[1]

The star is located north of the globular cluster NGC 4372, but it is much closer to earth than this cluster of stars, at a distance of about 101 parsecs (330 light-years).[1] NGC 4372 is 5,800 parsecs (19,000 ly) away.[7]

The host star TOI-1227 is part of a subgroup of the Lower Centaurus Crux OB association, sometimes called B,[6] A0[4] and called Musca group by the scientists that discovered TOI-1227 b. This group was called Musca after the constellation Musca in which most of its members are located.[1]

TOI-1227 has a spectral type of M4.5V to M5V, a mass 17% of the Sun and a radius 56% of the Sun. The host star is relative faint for a TOI with a visual magnitude of about 17.[1] The right ascension of 12h 27m 4.31s and the declination −72° 27′ 6.5″ implies that it is located in the Musca constellation.[2][c] The host star shows Lithium in its atmosphere, which should be depleted within 10-200 million years for M-dwarfs.[1]

References

[edit]
  1. ^ a b c d e f g h i j k l m Mann, Andrew W.; Wood, Mackenna L.; Schmidt, Stephen P.; Barber, Madyson G.; Owen, James E.; Tofflemire, Benjamin M.; Newton, Elisabeth R.; Mamajek, Eric E.; Bush, Jonathan L.; Mace, Gregory N.; Kraus, Adam L.; Thao, Pa Chia; Vanderburg, Andrew; Llama, Joe; Johns-Krull, Christopher M. (2022-04-01). "TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux". The Astronomical Journal. 163 (4): 156. arXiv:2110.09531. Bibcode:2022AJ....163..156M. doi:10.3847/1538-3881/ac511d. ISSN 0004-6256. S2CID 239024522.
  2. ^ a b c d e "TOI-1227". simbad.cds.unistra.fr. Retrieved 2024-02-14.
  3. ^ a b c d e f "TOI-1227 | NASA Exoplanet Archive". exoplanetarchive.ipac.caltech.edu. Retrieved 2024-02-14.
  4. ^ a b Goldman, Bertrand; Röser, Siegfried; Schilbach, Elena; Moór, Attila C.; Henning, Thomas (2018-11-01). "A Large Moving Group within the Lower Centaurus Crux Association". The Astrophysical Journal. 868 (1): 32. arXiv:1807.02076. Bibcode:2018ApJ...868...32G. doi:10.3847/1538-4357/aae64c. ISSN 0004-637X. S2CID 119343278.
  5. ^ Zari, E.; Hashemi, H.; Brown, A. G. A.; Jardine, K.; de Zeeuw, P. T. (2018-12-01). "3D mapping of young stars in the solar neighbourhood with Gaia DR2". Astronomy and Astrophysics. 620: A172. arXiv:1810.09819. Bibcode:2018A&A...620A.172Z. doi:10.1051/0004-6361/201834150. ISSN 0004-6361. S2CID 119078481.
  6. ^ a b Kerr, Ronan M. P.; Rizzuto, Aaron C.; Kraus, Adam L.; Offner, Stella S. R. (2021-08-01). "Stars with Photometrically Young Gaia Luminosities Around the Solar System (SPYGLASS). I. Mapping Young Stellar Structures and Their Star Formation Histories". The Astrophysical Journal. 917 (1): 23. arXiv:2105.09338. Bibcode:2021ApJ...917...23K. doi:10.3847/1538-4357/ac0251. ISSN 0004-637X. S2CID 234790391.
  7. ^ Boyles, Jason; Lorimer, Duncan R.; Turk, Phil J.; Mnatsakanov, Robert; Lynch, Ryan S.; Ransom, Scott M.; Freire, Paulo C.; Belczynski, Khris (2011-11-20). "Young Radio Pulsars in Galactic Globular Clusters". The Astrophysical Journal. 742 (1): 51. arXiv:1108.4402. doi:10.1088/0004-637X/742/1/51. ISSN 0004-637X.
  1. ^ For comparison, the Solar System is about 4.6 billion years old.
  2. ^ Calculated using an apparent magnitude of 17 and a distance of 100.641 parsecs[3] in the equation Mapp = Mabs - 5 + 5 * log(distance (parsecs))
  3. ^ The constellation can be obtained by the right ascension and declination in this website.
  1. ^ Obtained with a right ascension of 12h 27m 4.31s and a declination of −72° 27′ 6.5″[2] on this website.
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