SDSS J1416+1348: Comparison
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Coordinates: 14h 16m 24.08s, +13° 48′ 26.7″ SDSS J1416+1348 (full designation is SDSS J141624.08+134826.7) is a nearby wide binary system of two brown dwarfs, located in constellation Boötes. The system consists of L-type component A and T-type component B.

  • 24.08s
  • binary system
  • j141624.08134826.7

1. Discovery

Component A was discovered in late 2009[1] from a search of Sloan Digital Sky Survey (SDSS) Data Release 7, an astronomical survey conducted at Apache Point Observatory in New Mexico, United States . It has two discovery papers: Bowler et al., 2009[2] and Schmidt et al., 2009.[3]

Component B was discovered in early 2010 from UKIDSS Large Area Survey (ULAS) Data Release 5[4] & 6,[5] an astronomical survey conducted on the United Kingdom Infrared Telescope (UKIRT) on Mauna Kea in Hawaii. It has also two discovery papers: Burningham et al., 2010[4] and Scholz, 2010.[5] Burningham et al. discovered the whole system (independently of Bowler et al. and Schmidt et al.[4]) by cross-matching the ULAS DR5 against SDSS DR7,[4] and Scholz discovered component B by inspecting the UKIDSS finding charts around already found component A.[5]

2. Distance

In 2012 was published the first relatively precise parallax of SDSS J1416+1348, measured at the Canada-France-Hawaii Telescope under The Hawaii Infrared Parallax Program: 109.9 ± 1.8 mas, corresponding to a distance 9.10 ± 0.15 pc (29.7 ± 0.5 ly).[6] (Although, two parallaxes with large errors was previously published by Bowler et al.[2] and Scholz[5]).

SDSS J1416+1348 distance estimates
SourceParallax, masDistance, pcDistance, lyRef.
Bowler et al., 2009107 ± 34[7]9.3+4.4−2.330.5+14.2−7.6[2]
Bowler et al., 2009 8.4 ± 1.927.4 ± 6.2[2]
Schmidt et al., 2009 8.0 ± 1.626.1 ± 5.2[3]
Burningham et al., 2010 5–1516–49[4]
Scholz, 2010 7.9 ± 1.725.8 ± 5.5[5]
Burgasser et al., 2010 10.6+3.0−2.834.6+9.8−9.1[8]
Cushing et al., 2010 9.7 ± 0.1[9]31.6 ± 0.3[9][10]
The Hawaii Infrared Parallax Program

(Dupuy & Liu, 2012)		109.9 ± 1.89.10 ± 0.1529.7 ± 0.5[6]

SDSS J1416+1348 distance estimates

 
SourceParallax, masDistance, pcDistance, lyRef.
Bowler et al., 2009107 ± 34[7]9.3+4.4−2.330.5+14.2−7.6[2]
Bowler et al., 2009 8.4 ± 1.927.4 ± 6.2[2]
Schmidt et al., 2009 8.0 ± 1.626.1 ± 5.2[3]
Burningham et al., 2010 5–1516–49[4]
Scholz, 2010 7.9 ± 1.725.8 ± 5.5[5]
Burgasser et al., 2010 10.6+3.0−2.834.6+9.8−9.1[8]
Cushing et al., 2010 9.7 ± 0.1[9]31.6 ± 0.3[9][10]
The Hawaii Infrared Parallax Program

(Dupuy & Liu, 2012)		109.9 ± 1.89.10 ± 0.1529.7 ± 0.5[6]

Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.

3. Space Motion

SDSS J1416+1348 has proper motion 165 mas·yr−1 with position angle 32 degrees, indicating motion in north-east direction on the sky. Corresponding right ascension and declination components of proper motion are 88.0 ± 2.8 mas/yr and 139.9 ± 1.3 mas/yr, respectively.[3] At distance 29.7 ly (assuming parallax 109.0 ± 1.8 mas),[6] corresponding tangential velocity is 7.1 km/s. Radial velocity of SDSS J1416+1348 is -42.2 ± 5.1 km/s.[3] (Negative radial velocity value indicates that SDSS J1416+1348 is now approaching to us). Total velocity of SDSS J1416+1348 relatively to Solar system is 42.8 km/s.

SDSS J1416+1348 space motions estimates

Sourceμ,

mas/yr		P. A.,

°		μRA,

mas/yr		μDEC,

mas/yr		Vtan,

km/s[11]		Vr,

km/s		Ref.
Bowler et al., 2009151 ± 833 ± 4821276.5–38 ± 10[2]
Schmidt et al., 20091653288.0 ± 2.8139.9 ± 1.37.1-42.2 ± 5.1[3]
Scholz, 20101633286.2 ± 2.6138.8 ± 2.67.1 [5]
SIMBAD1653288 ± 3140 ± 27.1-87 ± 33[12]
Dupuy & Liu, 2012161.3 ± 2.836.1 ± 1.295.1 ± 3.0130.3 ± 3.07.1 [6]

The most accurate estimates are marked in bold.

Space motion of SDSS J1416+1348 indicates that it is member of Galactic thin disk population.[2][3][5]

3.1. Solar Encounter

Since SDSS J1416+1348 moves much faster in radial direction than in tangential direction, and radial velocity is negative, this brown dwarf system should pass Solar system in future at much smaller distance, than today's distance. Proper motion and radial velocity values from Schmidt et al., 2009 and parallax from Dupuy & Liu, 2012, assuming motion with constant velocity along straight line, yield minimal distance 4.9 ly circa year 207100.

Solar encounter chronology, assuming motion with constant velocity in a straight line relatively Solar system:[13]

DateDistance,

ly		ConstellationNote
759300 BC137.96Virgo/Boötestransition to constellation Boötes
493000 BC100Boötesapproach to a distance of 100 ly
141600 BC50Boötesapproach to a distance of 50 ly
300 BC30Boötesapproach to a distance of 30 ly
200029.68Boötesnear present time
7130020Boötesapproach to a distance of 20 ly
10790015Boötesapproach to a distance of 15 ly
14620010Boötesapproach to a distance of 10 ly
1629008.01Boötes/Corona Borealistransition to constellation Corona Borealis
1680007.46Corona Borealis/Boötestransition to constellation Boötes
1706007.18Boötes/Herculestransition to constellation Hercules
1865005.76Hercules/Dracotransition to constellation Draco
2020005Dracoapproach to a distance of 5 ly
2036004.97Draco/Cygnustransition to constellation Cygnus
2071004.95Cygnusminimal distance
2076004.95Cygnus/Cepheustransition to constellation Cepheus
2122005Cepheusremoval to a distance of 5 ly
2128005.01Cepheus/Cygnustransition to constellation Cygnus
2153005.08Cygnus /Cepheustransition to constellation Cepheus
2156005.09Cepheus/Lacertatransition to constellation Lacerta
2225005.41Lacerta/Andromedatransition to constellation Andromeda
2623009.3Andromeda/Piscestransition to constellation Pisces
26800010Piscesremoval to a distance of 10 ly
30640015Piscesremoval to a distance of 15 ly
34300020Piscesremoval to a distance of 20 ly
41050029.44Pisces/Cetustransition to constellation Cetus
41450030Cetusremoval to a distance of 30 ly
50700043.07Cetustransition to southern hemisphere
55590050Cetusremoval to a distance of 50 ly
907200100Cetusremoval to a distance of 100 ly

4. System's Properties

SDSS J1416+1348 is an old system (age estimates: >0.8 Gyr,[3] ~10 Gyr,[4] ~5 Gyr,[5] 2–10 Gyr,[8] >3.2 Gyr[10]), and, probably, possesses low metallicity.[4] Its two components are separated at angular distance 9.81 arcsec, corresponding to a projected separation 89.3 ± 1.5 a. u.[6] The system's orbit semi-major axis estimate is 104+28−72 a. u.[6]

4.1. Component A

The primary (brighter) component (SDSS J141624.08+134826.7 is mainly its designation; also known as SDSS J1416+13A) is a brown dwarf of spectral type sdL7,[14] or L6,[2][5][6] or L5,[3] or d/sdL7.[4] It has unusually blue near-infrared J−KS color.[3][4][5][8] According to Cushing et al. 2010, its peculiar spectrum is primarily a result of thin condensate clouds, and also vertical mixing occurs in its atmosphere.[10] However, in Burgasser et al., 2010 it was suggested that its (as well as component's B) peculiarities arise from age or metallicity, rather than cloud properties alone (since both A and B components have common peculiarities).[8]

4.2. Component B

The secondary (fainter) component (ULAS J141623.94+134836.3, abbreviated to ULAS J1416+1348, also known as SDSS J1416+13B) is a brown dwarf of spectral type T7.5,[8][15][16] or T7.5p.[4][6] It has unusually extremely blue near-infrared color H−K,[4] very red optical-to-near-infrared color (z−Y > +2.3 and z−J > +3.1),[5] and extremely red color H−[4.5] = 4.86 ± 0.04[4] (it was suggested, that the latter may be explained by presence of a cooler unresolved companion to SDSS J1416+13B).[4] Also, its spectrum indicates high surface gravity and/or subsolar metallicity.[8]

References

  1. Date of arXiv preprint. The articles was published in journals in early 2010.
  2. Bowler, Brendan P.; Liu, Michael C.; Dupuy, Trent J. (2010). "SDSS J141624.08+134826.7: A Nearby Blue L Dwarf From the Sloan Digital Sky Survey". The Astrophysical Journal 710 (1): 45–50. doi:10.1088/0004-637X/710/1/45. Bibcode: 2010ApJ...710...45B.  https://dx.doi.org/10.1088%2F0004-637X%2F710%2F1%2F45
  3. Schmidt, Sarah J.; West, Andrew A.; Burgasser, Adam J.; Bochanski, John J.; Hawley, Suzanne L. (2010). "Discovery of an Unusually Blue L Dwarf Within 10 pc of the Sun". The Astronomical Journal 139 (3): 1045–1050. doi:10.1088/0004-6256/139/3/1045. Bibcode: 2010AJ....139.1045S.  https://dx.doi.org/10.1088%2F0004-6256%2F139%2F3%2F1045
  4. Burningham, Ben; Leggett, S. K.; Lucas, P. W.; Pinfield, D. J.; Smart, R. L.; Day-Jones, A. C. et al. (2010). "The discovery of a very cool binary system". Monthly Notices of the Royal Astronomical Society 404 (4): 1952–1961. doi:10.1111/j.1365-2966.2010.16411.x. Bibcode: 2010MNRAS.404.1952B.  https://dx.doi.org/10.1111%2Fj.1365-2966.2010.16411.x
  5. Scholz, R.-D. (2010). "ULAS J141623.94+134836.3 - a faint common proper motion companion of a nearby L dwarf. Serendipitous discovery of a cool brown dwarf in UKIDSS DR6". Astronomy and Astrophysics 510: L8. doi:10.1051/0004-6361/201014078. Bibcode: 2010A&A...510L...8S.  https://dx.doi.org/10.1051%2F0004-6361%2F201014078
  6. Schmidt, Sarah J.; West, Andrew A.; Burgasser, Adam J.; Bochanski, John J.; Hawley, Suzanne L. (2010). "Discovery of an Unusually Blue L Dwarf Within 10 pc of the Sun". The Astronomical Journal 139 (3): 1045–1050. doi:10.1088/0004-6256/139/3/1045. Bibcode: 2010AJ....139.1045S.
  7. Relative parallax.
  8. Burgasser, Adam J.; Looper, Dagny; Rayner, John T. (2010). "ULAS J141623.94+134836.3: A Blue T Dwarf Companion to a Blue L Dwarf". The Astronomical Journal 139 (6): 2448–2454. doi:10.1088/0004-6256/139/6/2448. Bibcode: 2010AJ....139.2448B.  https://dx.doi.org/10.1088%2F0004-6256%2F139%2F6%2F2448
  9. The error does not include any errors in temperature and surface gravity and therefore is actually larger.
  10. Cushing, Michael C.; Saumon, D.; Marley, Mark S. (2010). "SDSS J141624.08+134826.7: Blue L dwarfs and Non-equilibrium Chemistry". The Astronomical Journal 140 (5): 1428–1432. doi:10.1088/0004-6256/140/5/1428. Bibcode: 2010AJ....140.1428C.  https://dx.doi.org/10.1088%2F0004-6256%2F140%2F5%2F1428
  11. Assuming parallax 109.9 ± 1.8 mas.
  12. "2MASS J14162408+1348263 -- Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.cfa.harvard.edu/simbad/sim-id?submit=display&bibdisplay=refsum&bibyear1=1850&bibyear2=%24currentYear&Ident=%405197735&Name=2MASS+J14162408%2B1348263#lab_bib. Retrieved 2012-05-19. 
  13. Actually, galactic orbits may be considered as approximately straight lines only on a scale much smaller than theirs sizes.
  14. Kirkpatrick, J. Davy; Looper, Dagny L.; Burgasser, Adam J.; Schurr, Steven D.; Cutri, Roc M.; Cushing, Michael C. et al. (2010). "Discoveries from a Near-infrared Proper Motion Survey Using Multi-epoch Two Micron All-Sky Survey Data". The Astrophysical Journal Supplement 190 (1): 100–146. doi:10.1088/0067-0049/190/1/100. Bibcode: 2010ApJS..190..100K. http://authors.library.caltech.edu/20570/1/Kirkpatrick2010p11580Astrophys_J_Suppl_S.pdf. 
  15. Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L. et al. (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal 753: 156. doi:10.1088/0004-637X/753/2/156. Bibcode: 2012ApJ...753..156K.  https://dx.doi.org/10.1088%2F0004-637X%2F753%2F2%2F156
  16. Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A. et al. (2011). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement 197 (2): 19. doi:10.1088/0067-0049/197/2/19. Bibcode: 2011ApJS..197...19K.  https://dx.doi.org/10.1088%2F0067-0049%2F197%2F2%2F19
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