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词条 WISE 1217+1626
释义

  1. History of observations

     Discovery  Initial estimate of spectral type  Discovery of component B 

  2. Distance

  3. Space motion

  4. Physical properties

  5. See also

  6. Notes

  7. References

{{Sky|12|17|56.96|+|16|26|39.98|34.2}}{{Starbox begin
|name=WISEPC J121756.91+162640.2}}{{Starbox observe
|epoch=MJD 55549.01{{r|Kirkpatrick2011}}
|equinox=J2000{{r|Kirkpatrick2011}}
|constell=Coma Berenices
|ra={{RA|12|17|56.96}}{{r|Kirkpatrick2011}}
|dec={{DEC|16|26|39.98}}{{r|Kirkpatrick2011}}}}{{Infobox|child=yes
| header1 =
Characteristics

| header2 = Whole system
| label3 = Apparent magnitude (Y (MKO filter system)
| data3 = {{val|18.38|0.04}}{{r|Liu2012}}
| label4 = Apparent magnitude (J (2MASS filter system)
| data4 = >18.52{{r|Kirkpatrick2011}}
| label5 = Apparent magnitude (J (MKO filter system)
| data5 = {{val|17.83|0.02}}{{r|Kirkpatrick2011|Liu2012}}
| label6 = Apparent magnitude (H (2MASS filter system)
| data6 = >17.50{{r|Kirkpatrick2011}}
| label7 = Apparent magnitude (H (MKO filter system)
| data7 = {{val|18.18|0.05}}{{r|Kirkpatrick2011|Liu2012}}
| label8 = Apparent magnitude (KS (2MASS filter system)
| data8 = >16.64{{r|Kirkpatrick2011}}
| label9 = Apparent magnitude (K (MKO filter system)
| data9 = {{val|18.80|0.04}}{{r|Liu2012}}
| header10 = Component A
| label11 = Spectral type
| data11 = T9{{r|Liu2012}}
| label12 = Apparent magnitude (Y (MKO filter system)
| data12 = {{val|18.59|0.04}}{{r|Liu2012}}
| label13 = Apparent magnitude (J (MKO filter system)
| data13 = {{val|17.98|0.02}}{{r|Liu2012}}
| label14 = Apparent magnitude (H (MKO filter system)
| data14 = {{val|18.31|0.05}}{{r|Liu2012}}
| label15 = Apparent magnitude (K (MKO filter system)
| data15 = {{val|18.94|0.04}}{{r|Liu2012}}
| header16 = Component B
| label17 = Spectral type
| data17 = Y0{{r|Liu2012}}
| label18 = Apparent magnitude (Y (MKO filter system)
| data18 = {{val|20.26|0.04}}{{r|Liu2012}}
| label19 = Apparent magnitude (J (MKO filter system)
| data19 = {{val|20.08|0.03}}{{r|Liu2012}}
| label20 = Apparent magnitude (H (MKO filter system)
| data20 = {{val|20.51|0.06}}{{r|Liu2012}}
| label21 = Apparent magnitude (K (MKO filter system)
| data21 = {{val|21.10|0.12}}{{r|Liu2012}}
}}{{Starbox astrometry
|prop_mo_ra={{val|786|42}}{{r|Dupuy2013}}
|prop_mo_dec={{val|-1224|27}}{{r|Dupuy2013}}
|parallax=99
|p_error=16
|parallax_footnote={{r|Dupuy2013}}
}}{{Starbox orbit
|reference={{r|Liu2012}}
|primary=A
|name=B
|period={{val|120|+220|-30}}—{{val|210|+380|-50}}
}}{{Starbox detail
|component1=Component A
|mass_mj=({{val|11.5|1.1}})—({{val|35|3}}){{r|Liu2012}}
|luminosity_bolometric=10−5.95 ± 0.18{{r|Liu2012}}
|gravity=({{val|4.39|0.03}})—({{val|5.07|0.05}}){{r|Liu2012}}
|temperature=({{val|490|30}})—({{val|660|40}}){{r|Liu2012}}
|component2=Component B
|mass_mj2=({{val|5.5|1.2}})—({{val|20|2}}){{r|Liu2012}}
|luminosity_bolometric2=10−6.79 ± 0.18{{r|Liu2012}}
|gravity2=({{val|4.07|0.10}})—({{val|4.77|0.05}}){{r|Liu2012}}
|temperature2=({{val|350|40}})—({{val|470|30}}){{r|Liu2012}}}}{{Starbox relpos
| epoch = UT 2012 January 29
| primary = A
| component = B
| angdistmas = {{val|758.2|1.4}}
| angdistref = {{r|Liu2012}}
| posang = {{val|14.50|0.13}}
| posangref = {{r|Liu2012}}
| projsep = ~ 8
| projsepref = {{r|Liu2012}}
}}{{Starbox catalog
|names=WISEPC J121756.91+162640.2{{r|Kirkpatrick2011}}
WISE J1217+1626{{r|Kirkpatrick2011|Liu2012}}
WISE 1217+1626{{r|Kirkpatrick2011}}
WISE J1217+1626AB{{r|Liu2012}}
}}{{Starbox reference
| Simbad = WISE+J1217%2B1626
}}{{Starbox end}}

WISEPC J121756.91+162640.2 (designation abbreviated to WISE 1217+1626, or WISE J1217+1626) is a binary brown dwarf system of spectral classes T9 + Y0,{{r|Liu2012}} located in constellation Coma Berenices at approximately 33 light-years from Earth.{{r|Dupuy2013}}

History of observations

Discovery

WISE 1217+1626 A was discovered in 2011 by J. Davy Kirkpatrick et al. from data, collected by Wide-field Infrared Survey Explorer (WISE) Earth-orbiting satellite — NASA infrared-wavelength 40 cm (16 in) space telescope, which mission lasted from December 2009 to February 2011. In 2011 Kirkpatrick et al. published a paper in The Astrophysical Journal Supplement, where they presented discovery of 98 new found by WISE brown dwarf systems with components of spectral types M, L, T and Y, among which also was WISE 1217+1626.{{r|Kirkpatrick2011}}[1]

Initial estimate of spectral type

Initial estimate of WISE 1217+1626' spectral type (before discovery of its binarity) was T9{{r|Kirkpatrick2011|Kirkpatrick2012}} (the same as the component's A type estimate made after this discovery).{{r|Liu2012}}

Discovery of component B

WISE 1217+1626 B was discovered in 2012 by Liu et al. with laser guide star (LGS) adaptive optics (AO) system of the 10-m Keck II Telescope on Mauna Kea, Hawaii, using infrared camera NIRC2 (the observations were made on 2012 January 29 (UT)). On 2012 April 1 (UT) Liu et al. observed WISE J1217+1626AB using the near-IR camera NIRI on the Gemini-North 8.1-m telescope on Mauna Kea, Hawaii and the binary was marginally resolved. On 12 April 2012 (UT) they obtained resolved spectroscopy of WISE J1217+1626AB with the near-IR spectrograph NIRSPEC again on the Keck II Telescope. In 2012 Liu et al. published a paper in The Astrophysical Journal where they presented results of observations with Keck II LGS-AO of three brown dwarf binary systems, binarity of one of which was known before, and binarity of the other two, including WISE 1217+1626, was first presented in this paper.{{r|Liu2012}}

Distance

Currently the most accurate distance estimate of WISE 1217+1626 is a trigonometric parallax, measured using Spitzer Space Telescope and published in 2013 by Trent Dupuy and Adam Kraus: 0.099 ± 0.016 arcsec, corresponding to a distance 10.1{{±|1.9|1.4}} pc, or 32.9{{±|6.4|4.6}} ly.{{r|Dupuy2013}} In the estimates made before discovery of the component's B by Liu et al. in 2012 the binarity is not taken into account.

WISE 1217+1626 distance estimates
Source Parallax, mas Distance, pc Distance, ly Ref.
Kirkpatrick et al. (2011)
(not assuming binarity) 		~6.7 ~21.9 Kirkpatrick2011}}
Kirkpatrick et al. (2012)
(not assuming binarity) 		~7.1 ~23.2 Kirkpatrick2012}}
Liu et al. (2012) 10.5 ± 1.7 34.2 ± 5.5 Liu2012}}
Dupuy & Kraus (2013) 99 ± 16[2] {{val>10.1|+1.9|-1.4}}{{val>32.9|+6.4|-4.6}}Dupuy2013}}
Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.

Space motion

WISE 1217+1626 has proper motion of about 1455 milliarcseconds per year.{{r|Dupuy2013}}

WISE 1217+1626 proper motion estimates
Source μ,
mas/yr 		P. A.,
° 		μRA,
mas/yr 		μDEC,
mas/yr 		Ref.
Kirkpatrick et al. (2011) 1765 148 935|269}}-1497|279}}Kirkpatrick2011}}
Dupuy & Kraus (2013) {{val>1455|38}}{{val>147.3|1.3}}{{val>786|42}}{{val>-1224|27}}Dupuy2013}}
The most accurate estimates are marked in bold.

Physical properties

Using three models, Liu et al. calculated physical properties of WISE 1217+1626 components.{{r|Liu2012}}

From Burrows et al. (2003) models and M(J):

Component and
assumed age 		{{Jupiter mass>Jup=y|link=y Teff,
K 		log g,
cm/s2 		P,
yr
A (for 1 Gyr) 11.5|1.1}}490|30}}4.39|0.03}}
B (for 1 Gyr) 7.4|0.5}}381|13}}4.18|0.03}}210|+370|-50}}
A (for 5 Gyr) 29|3}}530|30}}4.95|0.05}}
B (for 5 Gyr) 18.4|1.0}}402|11}}4.68|0.03}}130|+230|-30}}

From Lyon/COND models and M(J):

Component and
assumed age 		{{Jupiter mass>Jup=y|link=y Teff,
K 		log g,
cm/s2 		P,
yr
A (for 1 Gyr) 14.4|1.8}}610|40}}4.54|0.07}}
B (for 1 Gyr) 35|3}}430|30}}4.27|0.05}}190|+340|-50}}
A (for 5 Gyr) 8.3|0.9}}660|40}}5.07|0.05}}
B (for 5 Gyr) 20|2}}470|30}}4.77|0.05}}120|+220|-30}}

From Lyon/COND models and Lbol:

Component and
assumed age 		{{Jupiter mass>Jup=y|link=y Teff,
K 		log g,
cm/s2 		P,
yr
A (for 1 Gyr) 13|3}}580|70}}4.47|0.10}}
B (for 1 Gyr) 5.5|1.2}}350|40}}4.07|0.10}}210|+380|-50}}
A (for 5 Gyr) 33|5}}630|70}}5.04|0.09}}
B (for 5 Gyr) 13|3}}370|50}}4.54|0.11}}130|+240|-30}}

See also

The other two brown dwarf binary systems, observed by Liu et al. with Keck II LGS-AO in 2012:{{r|Liu2012}}

  • WISE 1711+3500 (T8 + T9.5, binarity was newly discovered)
  • CFBDSIR 1458+10 (T9 + Y0, binarity was known before)

Notes

1. ^These 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries were published earlier (however, also listed in Kirkpatrick et al. (2011)) in Mainzer et al. (2011) and Burgasser et al. (2011), and the other discoveries were published later.
2. ^Relative parallax.
3. ^{{cite journal | authorlink=J. Davy Kirkpatrick | last=Kirkpatrick |first=J. Davy |author2=Cushing, Michael C. |author3=Gelino, Christopher R. |author4=Griffith, Roger L. |author5=Skrutskie, Michael F. |author6=Marsh, Kenneth A. |author7=Wright, Edward L. |author8=Mainzer, A. |author9=Eisenhardt, Peter R. |author10=McLean, Ian S. |author11=Thompson, Maggie A. |author12=Bauer, James M. |author13=Benford, Dominic J. |author14=Bridge, Carrie R. |author15=Lake, Sean E. |author16=Petty, Sara M. |author17=Stanford, S. A. |author18=Tsai, Chao-Wei |author19=Bailey, Vanessa |author20=Beichman, Charles A. |author21=Bloom, Joshua S. |author22=Bochanski, John J. |author23=Burgasser, Adam J. |author24=Capak, Peter L. |author25=Cruz, Kelle L. |author26=Hinz, Philip M. |author27=Kartaltepe, Jeyhan S. |author28=Knox, Russell P. |author29=Manohar, Swarnima |author30=Masters, Daniel |author31=Morales-Calderon, Maria |author32=Prato, Lisa A. |author33=Rodigas, Timothy J. |author34=Salvato, Mara |author35=Schurr, Steven D. |author36=Scoville, Nicholas Z. |author37=Simcoe, Robert A. |author38=Stapelfeldt, Karl R. |author39=Stern, Daniel |author40=Stock, Nathan D. |author41=Vacca, William D. | title=The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE) | date=2011 | journal=The Astrophysical Journal Supplement | volume=197 | issue=2 | pages=19 | arxiv=1108.4677v1 | doi=10.1088/0067-0049/197/2/19 | bibcode=2011ApJS..197...19K}}
4. ^{{cite journal | authorlink=J. Davy Kirkpatrick | last1=Kirkpatrick | last2=Gelino |first1=J. D. | first2=C. R. | last3=Cushing | first3=M. C. | last4=Mace | first4=G. N. | last5=Griffith | first5=R. L. | last6=Skrutskie | first6=M. F. | last7=Marsh | first7=K. A. | last8=Wright | first8=E. L. | last9=Eisenhardt | first9=P. R. | last10=McLean | first10=I. S. | last11=Mainzer | first11=A. K. | last12=Burgasser | first12=A. J. | last13=Tinney | first13=C. G. | last14=Parker | first14=S. | last15=Salter | first15=G. | title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function | year=2012 | journal=The Astrophysical Journal | volume=753 | issue=2 | pages=156 | arxiv=1205.2122 | doi=10.1088/0004-637X/753/2/156 | bibcode=2012ApJ...753..156K}}
5. ^{{cite journal | last=Liu |first=Michael C. |author2=Dupuy, Trent J. |author3=Bowler, Brendan P. |author4=Leggett, S. K. |author5=Best, William M. J. | title=Two Extraordinary Substellar Binaries at the T/Y Transition and the Y-band Fluxes of the Coolest Brown Dwarfs | year=2012 | journal=The Astrophysical Journal | volume=758 | issue=1 | pages=57 | arxiv=1206.4044 | doi=10.1088/0004-637X/758/1/57 | bibcode=2012ApJ...758...57L}}
6. ^{{Cite journal | doi = 10.1126/science.1241917| title = Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects| journal = Science| volume = 341| issue = 6153| pages = 1492–5| year = 2013| last1 = Dupuy | first1 = T. J.| last2 = Kraus | first2 = A. L.|arxiv = 1309.1422 |bibcode = 2013Sci...341.1492D | pmid=24009359}}

References

{{reflist|colwidth=30em|refs=[3][4][5][6]
}}{{Stars of Coma Berenices}}

6 : Binary stars|Brown dwarfs|T-type stars|Y-type stars|Coma Berenices (constellation)|WISE objects
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