Unconfirmed/Unpublished Planets Catalogue

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 15th October 2015, 3:18 am

Lazarus wrote:Corrected link http://arxiv.org/abs/1201.0668

Oh, thanks. I don't get why that URL has been pasted there... Rolling Eyes
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 24th October 2015, 11:18 am

Browsing EPE Bibliography I've stumbled upon some old papers concerning very low-mass (<0.03 MSol) eclipsing companions of neutron stars. Is EPE going to treat them as "planets"?

http://exoplanet.eu/bibliography/

Notably PSR J2051-0827 (*LY Aqr) B and a ca. 9-10 MJ secondary of a pulsar in NGC 6544 globular cluster. But weren't they supposed to be treated as very low-mass degenerate stars?

The starting point from this recently submitted paper, I guess.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 28th November 2015, 5:28 am

Old news (2012) but worth reposting. Possibility of a dust cloud or a substellar companion (or a photoevaporating planet?) around carbon Mira-type star R Fornacis

Detection of an asymmetry in the envelope of the carbon Mira R Fornacis using VLTI/MIDI

Aims: We present a study of the envelope morphology of the carbon Mira R For with VLTI/MIDI. This object is one of the few asymptotic giant branch (AGB) stars that underwent a dust-obscuration event. The cause of such events is still a matter of discussion. Several symmetric and asymmetric scenarios have been suggested in the literature.
Methods: Mid-infrared interferometric observations were obtained separated by two years. The observations probe different depths of the atmosphere and cover different pulsation phases. The visibilities and the differential phases were interpreted using GEM-FIND, a tool for fitting spectrally dispersed interferometric observations with the help of wavelength-dependent geometric models.
Results: We report the detection of an asymmetric structure revealed through the MIDI differential phase. This asymmetry is observed at the same baseline and position angle two years later. The observations are best simulated with a model that includes a uniform-disc plus a Gaussian envelope plus a point-source. The geometric model can reproduce both the visibilities and the differential phase signatures.
Conclusions: Our MIDI data favour explanations of the R For obscuration event that are based on an asymmetric geometry. We clearly detect a photocentre shift between the star and the strongly resolved dust component. This might be caused by a dust clump or a substellar companion. However, the available observations do not allow us to distinguish between the two options. The finding has strong implications for future studies of the geometry of the envelope of AGB stars: if this is a binary, are all AGB stars that show an obscuration event binaries as well? Or are we looking at asymmetric mass-loss processes (i.e. dusty clumps) in the inner part of a carbon-rich Mira?
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 14th December 2015, 11:09 am

I've stumbled upon this and I've found some interesting exoplanet candidates orbiting giant stars, some forming 2-planet systems.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 20th June 2016, 10:19 am

Waiting for their confirmation, here are some exoplanet candidates orbiting sdB stars from Tomomi Otani's PhD thesis:

A Search for Planets and Brown Dwarfs around Post Main Sequence Stars

So far, the most promising theory for the existence of subdwarf B (sdB) stars is that they were formed during binary star evolution. This research was conducted to test this theory by searching for companions around six sdB pulsators (V391 Peg, HS 0702+6043, EC 20117-4014, PG 1219+534, PG 0911+456, and PG 1613+426) using the Observed-minus-Calculated (O-C) method. A star’s position in space will wobble due to the gravitational forces of any companion. If the star is emitting a periodic signal, the orbital motion of the star around the system’s center of mass causes periodic changes in the light pulse arrival times. After obtaining the O-C diagrams for these stars, useful limits on suspected companions’ minimum masses and semimajor axes were calculated. In addition, “period vs. amplitude” and “mass vs. semimajor axis” modeling were conducted to investigate the ranges and combinations of possible companion masses and semimajor axes that are consistent with the observational data. For V391 Peg and HS0702+6043, companions noted in previous publications validated the method used in this research and confirmed their existence. The results of this study of both these targets yield the same masses and semimajor axes as the published ones, within the uncertainties. For EC20117-4014, current data show that there is a companion and the signal of a companion candidate was detected with higher than 90% of confidence level. However, there is still several possible mass and semimajor axis combinations of the companion star. For PG1219+534, current data suggest that there may be a companion, however, the no-companion possibility still cannot be eliminated. The results of this project discovered two new possible companion candidates to EC20117-4014 and PG1219+534, confirmed companions previously detected in V391 Peg and HS0702+6043, as well as provided preliminary evidence for companions to EC20117- 4014 and PG1219+534 at the will require further observation. Though still a small sample, these results suggest that planets might survive the post-main-sequence evolution of their parent stars.

The candidates are:

1) PG 1219+534 b (or KY UMa b): m=5 Mj, a=0.262 AUs
2) EC 20117-4014 (AB)b [or *V4640 Sgr (AB)b]*: m=13.91 Mj, a=0.468 AUs
3) PG 0911+456 b (or DT Lyn b): m=9.1 Mj, a=0.212 AUs
4) PG 1613+426 b (or *V1078 Her b): m=4 Mj, a=0.479 AUs

(*) The planet could be circumbinary.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 25th September 2016, 4:52 pm

Numerical modelling of the HD 115600 system to try and figure out if a planet is causing the observed eccentricity/offset of the debris disc. Best fit is a 7.8 Jupiter mass planet at 30 AU in an eccentric e=0.2 orbit.

Thilliez & Maddison "Numerical search for a potential planet sculpting the young disc of HD 115600"
http://arxiv.org/abs/1609.06801
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 19th October 2016, 5:35 am

Several imaged substellar companions previously classed as "brown dwarfs" might be included in Extrasolar Planet Encyclopaedia according to latest "exoplanet-VLM star" divide (i.e. m < 61 Mj). Here are some but the list is much longer:

- 1RXS J235133.3+312720 B - m = 32 Mj a = 119 AUs
- 2MASS J00413538-5621127 B (or b)* - m = 15 Mj a = 8.9 AUs (*) = quite a planet
- 2MASS J05352184-0546085 B* - m = 36 Mj a = 0.0398 AUs (*) = eclipse and radius measured (= transit).
- 2MASS J11011926-7732383 B (or b)* - m = 25 Mj a = 240 AUs (*) = quite a planet
- 2MASS J12171110-0311131 B - m << 40 Mj a = 2.1 AUs
- 2MASS J12255432-2739466 B - m = ca. 29 Mj a = 3.17 AUs
- 2MASS J13153094-2649513 B - m > 16 Mj a = 6.6 AUs
- 2MASS J15344984-2952274 B - m = 26.9 Mj a = 2.3 AUs
- 2MASS J21321145+1341584 B - m = 48 Mj a = 1.8 AUs
- 2MASS J22244381-0158521 B - m = 27 Mj a = 75 AUs
- DENIS-P J185950.9-370632 B - m = 13 Mj (!) a = 7.8 AUs
- G 196-3 B (or b)* - m = 15-20 Mj a = 320 AUs (*) = quite a planet
- G 204-39 B - m = 20-35 Mj a = 2,685 AUs
- Gliese 229 B (or b) - m = ca. 40 Mj a = ca. 40 AUs (inner "Ab" to be converted in "c")
- GJ 3629 B (or b) - m = 46 +/- 16 Mj a = 4.4 +/- 0.6 AUs
- GSC 08047-00232 B= m = 10-25 Mj a = 844 AUs
- HETE J1900-12455 B (or b) - m = 16 Mj (<<70 Mj) p = 0.0578 d a = 0.0033 AUs
- LHS 6176 B - m = 30-55 Mj a = 970 AUs
- LP 261-75 B* - m = 20 Mj a = 820 AUs (*) = quite a planet
- NLTT 20346 B - m = 55 Mj a = 7,700 AUs
- PHL 5038 B - m = ca. 60 Mj a = 55 AUs
- SDSS J080531.84+481233.0 B* - m = 48 Mj a = 0.76 AUs i = 89° (*) = confirmed via astrometry
- SDSS J153417.05+161546.1 B = m = 35 Mj a = 4 AUs
- SDSS J224953.47+004404.6 B - m = 22 Mj a = 19 AUs
- WL 13 C [or (AB)b] - m = 17-20 Mj a = 1,400 AUs
- Wolf 940 B - m = 30 Mj a = 395 AUs
- Wolf 1130 (Gliese 781) B - m = 20-50 Mj a = 2,985 AUs
- Xi UMa E* - m = 28-48 Mj a = 4,100 AUs  (*) = How would it be? Just Xi UMa (AB)b or [(AaAb)(BaBb)]b?
- Xi UMa Bb* - m = 38 Mj a = ca. 0.06 AUs (*)  Is there an epistellar BD and/or a longer period stellar companion?
- Zeta Delphini B - m = 50 Mj a = 907 AUs

Same for a few brown dwarf companions to white dwarfs/sdB/neutron stars, even wanting to discard or ignore the He/CO-WD hypothesis. To say:

- 1RXS J105010.3-140431 B (or b) - m = 15 Mj (!!) p = 0.0615 d a = 0.003 AUs
- 4U 0614+091 (*V1055 Ori) - m = 10 Mj p = 0.0211 d a = 0.00167 AUs
- 4U 1543-624 B* - m = 30 Mj p = 0.0126 d a = 0.00118 AUs (*) = regarded as CO white dwarf
- AL Comae B (or "Rosino-Zwicky Object b") - m = 47 Mj a < 0.003 AUs
- CPD-64° 481 B - m = 48 Mj p = 0.178 d a = 0.0049 AUs
- EG Cancri B - m = 30 Mj a < 0.003 AUs
- GD 552 B - m = 30 Mj p = 0.0715 d a = 0.0028 AUs
- GP Comae B (or b) - m = 9.6-42.8 Mj (!) p = 0.03234 d a = 0.0016 AUs i = 33-78°
- IGR J12580+0134 B* - m = 14-30 Mj p = 1,300 d? (*) = primary is a black hole
- IX Draconis B - m = 30 Mj p = 0.067 d a = 0.0029 AUs
- NGC 6440 X-2 B (or b) - m = 6.7 Mj p = 0.0398 d a = 0.00255 AUs
- NGC 6440C B (or b) - m = 0.1 Me p = ca. 21 d a = ca. 0.16 AUs
- PSR J1124-3653 B - m = 27 Mj p = 0.229 d a = 0.0082 AUs
- PSR J1311-3430 B (or b) - m = 8.2 Mj (!) p = 0.065 d a = 0.0035 AUs
- PSR J1446-4701 B - m = 19 Mj (!) p = 0.277 d a = 0.0093 AUs
- PSR J1502-6752 B (or b)* - m = 22 Mj p = 2.4844 d  a = 0.04 AUs (*) = long period for a He-WD
- PSR J1544+4937 B - m = 17 Mj p = 0.12 d a = 0.00537 AUs
- PSR J1701-3006E (M62E) B (or b)* - m = 31 Mj p = 0.158 d a = 0.0063 AUs (*) = In M62 Cluster
- PSR J1701-3006F (M62F) B (or b)* - m = 21 Mj p = 0.205 d a = 0.0075 AUs (*) = In M62 Cluster
- PSR J1810+1744 B - m = 35 Mj p = 0.15 d a = 0.0062 AUs
- PSR J2214+3000 B - m > 14 Mj p = 0.4166 d a = 0.0122 AUs
- PSR J2256-1024 B - m = 30 Mj p = 0.2125 d a = 0.0078 AUs
- SAX J1808.4-3658 (*V4580 Sgr) B - m = 50 Mj p = 0.088 d a = 0.00438 AUs
- SWIFT J1753.5-0127 B* - m = 20 Mj p = 0.133 d a = ca. 0.011 AUs (*) = primary is a black hole
- SWIFT J1756.9-2508 B (or b)- m = 7.7 Mj p = 0.0398 d a = 0.0024 AUs
- WD 0137-349 B* - m = 52 Mj p =0.0833 d a = 0.006 AUs (*) = It has atmosphere detected
- WD 0837+185 B - m = 25-30 Mj a = 0.175 d a = 0.006 AUs
- WD 1310-230 (*V396 Hya) B (or b) - m = 6.1-30.5 Mj (!) p = 0.045 d a = 0.0017 AUs i = 25-79°
- WX Ceti B - m = 47 Mj p =0.0582 d a = ca. 0.003 AUs
- XTE J0929-314 (BW Antliae) B - m = 8-10 Mj (!) p = 0.03 d a = 0.0021 AUs
- XTE J1751-305 B - m = 13-17 Mj p = 0.0294 d a = 0.0020893 AUs
- XTE J1807-294 B (or b) - m = 6.6-8.4 Mj (!) p = 0.02777 d a = 0.002 AUs i = 18-90°
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 19th October 2016, 12:32 pm

The distant brown dwarf component of ξ UMa is assigned the letter D in the WDS catalogue, C seems to be optical (Raghavan et al. 2010). Unhelpfully, D has also been used to represent the secondary component of the B subsystem (which would be more systematically called Bb). There are several pieces of evidence that suggest that Bb is actually a star in a nearly face-on orbit: the rotational velocity of Ba suggests a low inclination (assuming Ba is tidally-locked to Bb) and from the system dynamics an additional 0.5 solar masses is needed in addition to Ba to bring the B subsystem up to the correct mass, see Griffin (1998). The claimed third star in the B subsystem (Bc) has never been seen again since the original discovery observations.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 20th October 2016, 4:21 am

Lazarus wrote:The distant brown dwarf component of ξ UMa is assigned the letter D in the WDS catalogue, C seems to be optical (Raghavan et al. 2010). Unhelpfully, D has also been used to represent the secondary component of the B subsystem (which would be more systematically called Bb). There are several pieces of evidence that suggest that Bb is actually a star in a nearly face-on orbit: the rotational velocity of Ba suggests a low inclination (assuming Ba is tidally-locked to Bb) and from the system dynamics an additional 0.5 solar masses is needed in addition to Ba to bring the B subsystem up to the correct mass, see Griffin (1998). The claimed third star in the B subsystem (Bc) has never been seen again since the original discovery observations.

Thus former brown dwarf candidate Xi UMa Bb is actually a star in nearly face-on orbit, right? Excellent information.

Anyway it doesn't solve the matter about outer circumbinary brown dwarf Xi UMa D. In case of planetary designation would it be just Xi UMa (AB)b (practically excluding inner binary components) or a "tongue and keyboard-twister" Xi UMa [(AaAb)(BaBb)]b?? cyclops

As I am I'm adding a few more "exoplanet candidate" brown dwarfs and some stellar weirdos in ultra-compact X-ray binaries:

- 2MASS J03370359-1758079 B - m = 10-15 Mj a = 2.52 AUs
- 2MASS J12095613-1004008 B - m = 25 Mj a = 3.24 AUs
- 2MASS J1341-3052  B - m = 22 Mj a = 8.6 AUs
- PSR J0636+5129 B (or b) - m = 8 Mj (!) p = 0.067 d a = 0.0036 AUs
- PSR J1518+0204C B (or b) - m > 38 Mj p = 0.08682882865 d a = 0.0043 AUs
- SLX 1737-282 B - m = 5-30 Mj p = n/a (range = 10-60 min) 0.0008 < a < 0.0026 AUs i = 60-85°
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 23rd January 2017, 3:38 pm

Edasich wrote:Long period substellar companion at HD 211847 listed in "confirmed" exoplanet section:

http://exoplanet.eu/catalog/hd_211847_b/
Turns out it's a star (~0.15 solar masses) in a face-on orbit.

Moutou et al. (2017) "Eccentricity in planetary systems and the role of binarity: sample definition, initial results, and the system of HD 211847"
https://arxiv.org/abs/1701.05664

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 25th January 2017, 10:22 am

Lazarus wrote:Turns out it's a star (~0.15 solar masses) in a face-on orbit.

Moutou et al. (2017) "Eccentricity in planetary systems and the role of binarity: sample definition, initial results, and the system of HD 211847"
https://arxiv.org/abs/1701.05664

Long period massive substellar objects often turn out to be actually stars. I'm not going to miss it too much.

Edasich wrote:
- GP Comae B (or b) - m = 9.6-42.8 Mj (!) p = 0.03234 d a = 0.0016 AUs i = 33-78°
- WD 1310-230 (*V396 Hya) B (or b) - m = 6.1-30.5 Mj (!) p = 0.045 d a = 0.0017 AUs i = 25-79°

These ones have been listed in EPE as "planets", likely of degenerate kind:

http://exoplanet.eu/catalog/gp_com_b/
http://exoplanet.eu/catalog/v396_hya_b/

Most of orbital parameters have been left blank though.
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Re: Unconfirmed/Unpublished Planets Catalogue

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