SDSS_J1416+1348
SDSS J141624.08+134826.7
Wide binary system in the constellation Bootes
SDSS J141624.08+134826.7 (abbreviated SDSS J1416+1348) 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.
SDSS J1416+1348 A (bright object) and SDSS J1416+1348 B (faint red object above) Credit: legacy surveys | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Boötes |
| Right ascension | 14h 16m 24.0740s[1] |
| Declination | 13° 48′ 26.193″[1] |
| Characteristics | |
| A | |
| Spectral type | sdL7[2] |
| Apparent magnitude (r) | 20.69±0.04[3] |
| Apparent magnitude (i) | 18.38±0.01[3] |
| Apparent magnitude (z) | 15.92±0.01[3] |
| Apparent magnitude (Y) | 14.255±0.003[3] |
| Apparent magnitude (J) | 12.995±0.001[4] |
| Apparent magnitude (H) | 12.469±0.001[4] |
| Apparent magnitude (KS) | 12.053±0.001[4] |
| R−I color index | 2.31±0.04[5] |
| J−H color index | 0.55±0.01[5] |
| J−K color index | 1.03±0.03[2] |
| B | |
| Spectral type | T7.5p[5] |
| Apparent magnitude (Y) | 18.16±0.02[5] |
| Apparent magnitude (J) | 17.259±0.017[4] |
| Apparent magnitude (H) | 17.62±0.02[5] |
| Apparent magnitude (KS) | 18.93±0.17[5] |
| J−H color index | −0.3[4] |
| J−K color index | −1.7[4] |
| Astrometry | |
| Radial velocity (Rv) | −42.2±5.1[6] km/s |
| Proper motion (μ) | RA: 86.670±0.291[1] mas/yr Dec.: 127.953±0.198[1] mas/yr |
| Parallax (π) | 107.7375 ± 0.2163 mas[1] |
| Distance | 30.27 ± 0.06 ly (9.28 ± 0.02 pc) |
| Orbit[7] | |
| Primary | A |
| Companion | B |
| Semi-major axis (a) | 104+28 −72 a.u. |
| Details[8] | |
| Component A | |
| Mass | 60±18 MJup |
| Radius | 0.92±0.08 RJup |
| Luminosity (bolometric) | log(−4.18±0.011) L☉ |
| Surface gravity (log g) | 5.22±0.22 cgs |
| Temperature | 1694±74 K |
| Age | 0.5–10 Gyr |
| Component B | |
| Mass | 33±22 MJup |
| Radius | 0.94±0.16 RJup |
| Luminosity (bolometric) | log(−5.80±0.07) L☉ |
| Surface gravity (log g) | 4.83±0.51 cgs |
| Temperature | 660±62 K |
| Age | 0.5–10 Gyr |
| Position (relative to A) | |
| Component | B |
| Angular distance | 9.81″ [7] |
| Projected separation | 89.3±1.5 AU [7] |
| Other designations | |
| Component A: SDSS J141624.08+134826.7,[3][6] SDSS J1416+1348,[3] SDSS J1416+13A,[9] SDSS J1416+13,[5] SDSS 1416+13,[6] SDSS 141624,[10] 2MASS J14162408+1348263,[11] SOZ 3A,[11] WDS J14164+1348A[11] | |
| Component B: ULAS J141623.94+134836.30,[5] ULAS J141623.94+134836.3,[4] SDSS J141624.08+134826.7B,[12] ULAS J1416+1348,[13] SDSS J1416+1348B,[14] ULAS J1416+13,[5] SDSS J1416+13B,[9] SDSS 141624 b,[10] WISE J141623.94+134836.0,[15] SOZ 3B,[12] WDS J14164+1348B[12] | |
| Database references | |
| SIMBAD | data |
Component A was discovered in late 2009[note 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[3] and Schmidt et al., 2009.[6]
Component B was discovered in early 2010 from UKIDSS Large Area Survey (ULAS) Data Release 5[5] & 6,[4] 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[5] and Scholz, 2010.[4] Burningham et al. discovered the whole system (independently of Bowler et al. and Schmidt et al.[5]) by cross-matching the ULAS DR5 against SDSS DR7,[5] and Scholz discovered component B by inspecting the UKIDSS finding charts around already found component A.[4]
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).[7] (Although, two parallaxes with large errors was previously published by Bowler et al.[3] and Scholz[4]).
| Source | Parallax, mas | Distance, pc | Distance, ly | Ref. |
|---|---|---|---|---|
| Bowler et al., 2009 | 107 ± 34[note 2] | 9.3+4.4 −2.3 | 30.5+14.2 −7.6 | [3] |
| Bowler et al., 2009 | 8.4 ± 1.9 | 27.4 ± 6.2 | [3] | |
| Schmidt et al., 2009 | 8.0 ± 1.6 | 26.1 ± 5.2 | [6] | |
| Burningham et al., 2010 | 5–15 | 16–49 | [5] | |
| Scholz, 2010 | 7.9 ± 1.7 | 25.8 ± 5.5 | [4] | |
| Burgasser et al., 2010 | 10.6+3.0 −2.8 | 34.6+9.8 −9.1 | [13] | |
| Cushing et al., 2010 | 9.7 ± 0.1[note 3] | 31.6 ± 0.3[note 3] | [9] | |
| The Hawaii Infrared Parallax Program (Dupuy & Liu, 2012) | 109.9 ± 1.8 | 9.10 ± 0.15 | 29.7 ± 0.5 | [7] |
Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.
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.[6] At distance 29.7 ly (assuming parallax 109.0 ± 1.8 mas),[7] corresponding tangential velocity is 7.1 km/s. Radial velocity of SDSS J1416+1348 is -42.2 ± 5.1 km/s.[6] (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
| Source | μ, mas/yr | P. A., ° | μRA, mas/yr | μDEC, mas/yr | Vtan, km/s[note 4] | Vr, km/s | Ref. |
|---|---|---|---|---|---|---|---|
| Bowler et al., 2009 | 151 ± 8 | 33 ± 4 | 82 | 127 | 6.5 | –38 ± 10 | [3] |
| Schmidt et al., 2009 | 165 | 32 | 88.0 ± 2.8 | 139.9 ± 1.3 | 7.1 | -42.2 ± 5.1 | [6] |
| Scholz, 2010 | 163 | 32 | 86.2 ± 2.6 | 138.8 ± 2.6 | 7.1 | [4] | |
| SIMBAD | 165 | 32 | 88 ± 3 | 140 ± 2 | 7.1 | -87 ± 33 | [11] |
| Dupuy & Liu, 2012 | 161.3 ± 2.8 | 36.1 ± 1.2 | 95.1 ± 3.0 | 130.3 ± 3.0 | 7.1 | [7] |
The most accurate estimates are marked in bold.
Space motion of SDSS J1416+1348 indicates that it is member of Galactic thin disk population.[3][4][6]
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 the Solar System in the future at a 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 relative to the Solar System:[note 5]
| Date | Distance, ly | Constellation | Note |
|---|---|---|---|
| 759300 BC | 137.96 | Virgo/Boötes | transition to constellation Boötes |
| 493000 BC | 100 | Boötes | approach to a distance of 100 ly |
| 141600 BC | 50 | Boötes | approach to a distance of 50 ly |
| 300 BC | 30 | Boötes | approach to a distance of 30 ly |
| 2000 | 29.68 | Boötes | near present time |
| 71300 | 20 | Boötes | approach to a distance of 20 ly |
| 107900 | 15 | Boötes | approach to a distance of 15 ly |
| 146200 | 10 | Boötes | approach to a distance of 10 ly |
| 162900 | 8.01 | Boötes/Corona Borealis | transition to constellation Corona Borealis |
| 168000 | 7.46 | Corona Borealis/Boötes | transition to constellation Boötes |
| 170600 | 7.18 | Boötes/Hercules | transition to constellation Hercules |
| 186500 | 5.76 | Hercules/Draco | transition to constellation Draco |
| 202000 | 5 | Draco | approach to a distance of 5 ly |
| 203600 | 4.97 | Draco/Cygnus | transition to constellation Cygnus |
| 207100 | 4.95 | Cygnus | minimal distance |
| 207600 | 4.95 | Cygnus/Cepheus | transition to constellation Cepheus |
| 212200 | 5 | Cepheus | removal to a distance of 5 ly |
| 212800 | 5.01 | Cepheus/Cygnus | transition to constellation Cygnus |
| 215300 | 5.08 | Cygnus /Cepheus | transition to constellation Cepheus |
| 215600 | 5.09 | Cepheus/Lacerta | transition to constellation Lacerta |
| 222500 | 5.41 | Lacerta/Andromeda | transition to constellation Andromeda |
| 262300 | 9.3 | Andromeda/Pisces | transition to constellation Pisces |
| 268000 | 10 | Pisces | removal to a distance of 10 ly |
| 306400 | 15 | Pisces | removal to a distance of 15 ly |
| 343000 | 20 | Pisces | removal to a distance of 20 ly |
| 410500 | 29.44 | Pisces/Cetus | transition to constellation Cetus |
| 414500 | 30 | Cetus | removal to a distance of 30 ly |
| 507000 | 43.07 | Cetus | transition to southern hemisphere |
| 555900 | 50 | Cetus | removal to a distance of 50 ly |
| 907200 | 100 | Cetus | removal to a distance of 100 ly |
SDSS J1416+1348 is an old system (age estimates: >0.8 Gyr,[6] ~10 Gyr,[5] ~5 Gyr,[4] 2–10 Gyr,[13] >3.2 Gyr[9]), and, probably, possesses low metallicity.[5] Its two components are separated at angular distance 9.81 arcsec, corresponding to a projected separation 89.3 ± 1.5 a. u.[7] The system's orbit semi-major axis estimate is 104+28
−72 a. u.[7]
Component A
The primary (brighter) component (SDSS J141624.08+134826.7 is its full designation; also known as SDSS J1416+13A) is a brown dwarf of spectral type sdL7,[2] or L6,[3][4][7] or L5,[6] or d/sdL7.[5] It has unusually blue near-infrared J−KS color.[5][4][6][13] 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.[9] 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).[13]
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,[13][15][16] or T7.5p.[5][7] It has unusually extremely blue near-infrared color H−K,[5] very red optical-to-near-infrared color (z−Y > +2.3 and z−J > +3.1),[4] and extremely red color H−[4.5] = 4.86 ± 0.04[5] (it was suggested, that the latter may be explained by presence of a cooler unresolved companion to SDSS J1416+13B).[5] Also, its spectrum indicates high surface gravity and/or subsolar metallicity.[13]
- Relative parallax.
- The error does not include any errors in temperature and surface gravity and therefore is actually larger.
- Assuming parallax 109.9 ± 1.8 mas.
- Actually, galactic orbits may be considered as approximately straight lines only on a scale much smaller than theirs sizes.
- Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- 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" (PDF). The Astrophysical Journal Supplement. 190 (1): 100–146. arXiv:1008.3591. Bibcode:2010ApJS..190..100K. doi:10.1088/0067-0049/190/1/100. S2CID 15821313.
- 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. arXiv:0912.3796. Bibcode:2010ApJ...710...45B. doi:10.1088/0004-637X/710/1/45. S2CID 119300240.
- 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. arXiv:1001.2743. Bibcode:2010A&A...510L...8S. doi:10.1051/0004-6361/201014078. S2CID 119217549.
- 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. arXiv:1001.4393. Bibcode:2010MNRAS.404.1952B. doi:10.1111/j.1365-2966.2010.16411.x. S2CID 17310918.
- 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. arXiv:0912.3565. Bibcode:2010AJ....139.1045S. doi:10.1088/0004-6256/139/3/1045. S2CID 17213443.
- Dupuy, Trent J.; Liu, Michael C. (2012). "The Hawaii Infrared Parallax Program. I. Ultracool Binaries and the L/T Transition". The Astrophysical Journal Supplement Series. 201 (2): 19. arXiv:1201.2465v1. Bibcode:2012ApJS..201...19D. doi:10.1088/0067-0049/201/2/19. S2CID 119256363.
- Gonzales, Eileen C.; et al. (2020). "Retrieval of the d/sdL7+T7.5p Binary SDSS J1416+1348AB". The Astrophysical Journal. 905 (1). 46. arXiv:2010.01224. Bibcode:2020ApJ...905...46G. doi:10.3847/1538-4357/abbee2.
- 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. arXiv:1009.2802. Bibcode:2010AJ....140.1428C. doi:10.1088/0004-6256/140/5/1428. S2CID 118408214.
- Schneider, Jean. "Star : SDSS 141624". Extrasolar Planets Encyclopaedia. Retrieved 2012-05-19.[dead link]
- "2MASS J14162408+1348263 -- Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2012-05-19.
- 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. arXiv:1002.0645. Bibcode:2010AJ....139.2448B. doi:10.1088/0004-6256/139/6/2448. S2CID 53407706.
- Burgasser, Adam J.; Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Looper, Dagny L.; et al. (2011). "Fire Spectroscopy of Five Late-type T Dwarfs Discovered with the Wide-field Infrared Survey Explorer". The Astrophysical Journal. 735 (2): 116. arXiv:1104.2537. Bibcode:2011ApJ...735..116B. doi:10.1088/0004-637X/735/2/116. S2CID 19003973.
- Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Eisenhardt, Peter R.; McLean, Ian S.; Mainzer, Amanda K.; Burgasser, Adam J.; Tinney, C. G.; Parker, Stephen; Salter, Graeme (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal. 753 (2): 156. arXiv:1205.2122. Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156. S2CID 119279752.
- 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. arXiv:1108.4677v1. Bibcode:2011ApJS..197...19K. doi:10.1088/0067-0049/197/2/19. S2CID 16850733.