Unconfirmed/Unpublished Planets Catalogue

I never hear again about the Planet around LHS 288 a M dwarf star at 15.6 light years than was detect by astrometry, but not confirm yet...

http://en.wikipedia.org/wiki/LHS_288

http://www.astro.virginia.edu/~jlb2j/Dissertation/SStarsFinal.pdf

Thank you to remember us this one

Constraining the structure of the planet-forming region in the disk of the Herbig Be star HD 100546

Disc morphology can be explained by a 1-8 Jupiter masses planet at ~8 AU from HD 100546.

From Astronomy and Astrophysics "Forthcoming" list...

Quote :

A likely exoplanet orbiting the oscillating K-giant alpha Arietis
B.-C. Lee, D. E. Mkrtichian, I. Han, K.-M. Kim, M.-G. Park
Received: 10 December 2010 / Accepted: 10 March 2011

So much for Sirius C...

Piercing the Glare: Direct Imaging Search for Planets in the Sirius System

Lazarus wrote:

So much for Sirius C...

Piercing the Glare: Direct Imaging Search for Planets in the Sirius System

Once again astrometry finds something that actually does not exist. However there are still some possibilities...

Sirius is a difficult target, not really ideal for precision astrometry as it is too bright.

Amusing contrast with the various planets detected by the space-based transit surveys, which are hard to follow up because the stars are so dim.

The EPE has added an unconfirmed microlensing planet, OGLE-2008-BLG-513/MOA-2008-BLG-401, from this paper.

Discovered by microlensing planet is unconfirmed??strange?

Probably because no paper is available yet.

(Although EPE is not consistent in this... how are those 32 HARPS planets announced back in October 2009 coming along?)

Something to bear in mind when considering the case of the claimed companion of Epsilon Ursae Majoris (Alioth):

Modelling the light variability of the Ap star ɛ Ursae Majoris

The star has light variability arising from varying concentrations of various chemical elements across its surface and it has a rotation period of 5.1 days, the same as the claimed orbital period of the substellar companion. I therefore have to wonder whether the radial velocity variations might be arising due to processes intrinsic to the star, something which was only briefly addressed in Sokolov's paper.

Noticed that. But curiously the paper does not mention Sokolov's paper, neither rejects the proposed substellar companion...

And neither a further research paper has been so far provided

Here some cases of substellar objects with mass around or below the 25 Jupiter masses thresold established for the Extrasolar Planet Encyclopaedia. I hope these ones may be listed in the planet counter of EPE soon:

1) 17-20 Jupiter masses companion 1,400 AUs away from WL 13 (or VSSG 25), binary system with two M4 dwarfs. To be eventually labelled as WL 13 (AB)b or VSSG 25 (AB)b.

http://arxiv.org/abs/1106.0574


2) GSC 08047-00232 B, confirmed as 20 Mj object in Chauvin et al. (2010)

http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2010A%26A...509A..52C&db_key=AST&nosetcookie=1

3) WISEPC J045853.90+643451.9 AB, a T8.5+T9 system. Total mass 25 Jupiter masses and secondary equivalent to 10 Mj.

http://adsabs.harvard.edu/abs/2011AJ....142...57G

http://arxiv.org/abs/1106.3142

4) 2MASS J0041353-562112 - 30 Mj brown dwarf with low-mass companion (15 Jupiter masses) in Phoenix field.

http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014206&Itemid=129

5) LOri 167 - low mass binary with 17 and 5 Jupiter masses components in Orion

http://www.aanda.org/index.php?option=com_article&access=standard&Itemid=129&url=/articles/aa/pdf/2007/22/aa7258-07.pdf

6) HD 203030 B - optically imaged, mass 23 Jupiter masses

http://cdsbib.u-strasbg.fr/cgi-bin/cdsbib?2006ApJ...651.1166M

7) G 196-3 B - Latest mass estimate for G 196-3 provides range between 12 and 25 Jupiter masses (Zapatero-Osorio et al. 2010)

http://cdsbib.u-strasbg.fr/cgi-bin/cdsbib?2010ApJ...715.1408Z

SDSS J224953.47+004404.6 A & B - Binary brown dwarf with secondary at 22 Jupiter masses (Allers et al. 2010)

http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2010ApJ...715..561A&db_key=AST&nosetcookie=1

9) ScoPMS 214 or V2505 Oph B - 25 Mj companion 450 AUs away.

http://arxiv.org/abs/0808.2982
http://www.astro.sunysb.edu/metchev/PUBLICATIONS/thesis.pdf

According to this IOP paper (free access, hopefully), there are some late T-type object whose masses would well fall within 20-25 Jupiter masses upper limit set for EPE:

THE BROWN DWARF KINEMATICS PROJECT. II. DETAILS ON NINE WIDE COMMON PROPER MOTION VERY LOW MASS COMPANIONS TO NEARBY STARS

Here some interesting cases:


- CD-33° 7795 (or TWA 5) B: Who remembers this young M dwarf? It was featuring in Whatmough's EV Brown Dwarf section. The substellar companion also seems itself binary

- GSC 08047-00232 B, in Horologium-Tucana Association, I think. It would add to AB Pictoris b, wouldn't it?

- LP 261-75 B, in Leo Minor

- HD 203030 B in Vulpecula

Schneider has just added this paper to Bibliography section on August 11. Who knows if in fall August, these are going to feature in the list?

As I am, I add these young objects whose mass equates or is less than 20 Jupiter masses:

- 2MASS J11103481-7722053 B in Chamaeleo. Primary a dM4 (0.27 Solar masses) + secondary 20 Jupiter masses 1,535 AUs away.

I also have got the paper of Kraus & Hillenbrand (2007) with a full table of young stars with widely separated stellar and substellar companions. Oddly the same full table is not viewable in current fulltext of this paper. I don't know if there has been an embargo risk and original draft withdrawn.

http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2007ApJ...662..413K&db_key=AST&nosetcookie=1

It gives, say, star òò Tau with a 20 Mj companion and XXYY n with 10 Jupiter masses (Stellar objects intentionally hidden).
And many other cases very similar to 1RXS 1609 B.

You can PM me for details btw.

EDIT

Oddly arXiv preprint has the full table. Take a look

http://arxiv.org/abs/astro-ph/0702545

Always accounting new upper mass limit of EPE, so would this B subdwarf (EC 2210-1916) host a massive planetary companion, unless classed as Helium-WD (though inferred radius appears large enough to be planetary)

http://arxiv.org/abs/1104.4202

Quote :

Adopting the upper limits for P and K, the companion would have to be a brown dwarfwith ≃ 20M_J and a radius of ≃ 0.1R⊙. For inclinations lower than 90◦ the orbital periodof the putative binary must be shorter, because the absolute rotational velocity of the sdBhas to be higher to keep vrot sin i fixed at the observed value.

From slightly later in the EC 2210-1916 paper from where you quoted...

Quote :

These simple calculations show that the possible parameter space of a close and synchronised binary would be extremely narrow (P ≃ 0.1−0.15 d, K ≃ 4−12 km s⁻¹). Furthermore, all possible configurations would lead to photometric variabilities easily visible in the light curve. Close sdB+dM or BD systems are not only often eclipsing, but also show sinusoidal variations due to light from the irradiated surface of the cool companion (e.g. Østensen et al. 2010; For et al. 2010; Geier et al. 2011a). Due to its high temperature and low surface gravity EC 22018−1916 has a very high luminosity compared to other sdBs, which should lead to a very strong reflection effect at inclinations of ≃ 50° or higher. Since no variations were found in the ASAS and NSVS light curves (Figure 4), a nearby low-mass companion can be excluded as well.

(emphasis mine)

This would appear to be an exclusion of the planetary hypothesis...

Here some low-mass, imaged substellar companions whose mass should be now classed as "planetary". I think they should be included in Extrasolar Planet Encyclopaedia:

Imaged companions with masses between 8-25 Mj:

- WISEPC J045853.90+643451.9 B: m=10 Mj, a=5 AUs

- 2MASS J13153094-2649513 B: m>16 Mj, a=6.6 AUs

- DENIS-P J185950.9-370632 B: m=13 Mj, a=7.8 AUs

- 2MASS J00413538-5621127 B: m=15 Mj, a=8.9 AUs

- SDSS J224953.47+004404.6 B: m=22 Mj, a=19 AUs

- CD -33 7795 (or TWA 5) B: m=20 Mj, a=100 AUs (itself binary?)

- GSC 08047-00232 B: m=25 Mj, a=200 AUs

- 2MASS J11011926-7732383 B: m=25 Mj, a=240 AUs

- G 196-3 B: m=12-25 Mj, a=320 AUs

- HD 203030 B: m=23 Mj, a=487 AUs

- LP 261-75 B: m=20 Mj, a=820 AUs

- WL 13 (or VSSG 25) C (or (AB)b?): m=17-20 Mj, a=1,400 AUs

- LOri167 B: m=8 Mj, a=2,000 AUs


Others with mass around 25-30 Mj:

- 2MASS J15344984-2952274 B: m=26.9 Mj, a=2.3 AUs

- 2MASS J12255432-2739466 B: m=29 Mj, a=3.17 AUs

- 2MASS J22244381-0158521 B: m=27 Mj, a=75 AUs

- Wolf 940 B: m=28-30 Mj, a=395 AUs


Non-imaged, RV-detected:

- TYC 1240-945-1 B= m=26 Mj, a=0.068 AUs

- MARVELS-1 b: m=28 Mj, a=0.071 *transiting*

- HD 189310 B: m=25.6 Mj, a=0.107 AUs e=0.359

- 59 Draconis B: m=25 Mj, a=0.22 AUs, e=0.2


Substellar degenerates or planets?

- PSR B1957+20 (QX Sge) B: m=22 Mj, a=0.01388 AUs


If somebody wishes to e-mail this list to the EPE website, it's just welcome.

Hi

I find this on EPE. Have you more information about this star/planet?

http://exoplanet.eu/star.php?st=anonymous#a_publi

The only reference to that planet I know of is in this paper.

While reading this paper I came across an interesting paragraph.

Quote :

A complex two-month-long eclipse observed for the star 1SWASP J140747.93-394542.6 may have been due to a disk surrounding an otherwise-unknown planet, though it is also possible that the occulting disk instead adorns a low-mass stellar companion (Mamajek et al. 2011).

Anyone know anything more?
Edit: found reference to it here.

Perhaps in some respects similar to Epsilon Aurigae?

Existing thread

A curious case, worth to notify:

Zapatero Osorio et al. (2003) - Photometric variability of a young, low-mass brown dwarf

The brown dwarf S Ori 45 could host an undermassive secondary (9-13 Jupiter masses, and losing mass too) in epistellar orbit (0.002-0.003 AUs, P_orb=2.5-3.6 hours). Alternate explanations are possible, of course.

Possible hot Jupiter at TWA 13A

Precise Infrared Radial Velocities from Keck/NIRSPEC and the Search for Young Planets
http://arxiv.org/abs/1202.0300

Some interesting globular cluster neutron stars with undermassive companions (Lynch et al. 2012). Helium dwarfs or "PSR J1719-1438 b-like"?

PSR J1701-3006E (in M62) - m₂= 31 Jupiter masses; P_orb= 0.1584774951 d = 3.803 hrs
PSR J1701-3006F (in M62) - m₂= 21 Jupiter masses; P_orb= 0.2054870422 d = 4.932 hrs
PSR J1807−2459A (in NGC 6544) - m₂ = 0.0092 Solar = ca. 9.2 Jupiter masses; P_orb= 0.071091483516 d = 1.706 hrs

Paper links:

Preprint

Astrophysical Journal issue

Exoplanet around strange star appeared on EPE unconfirmed catalog
http://exoplanet.eu/planet.php?p1=PTFO+8-8695&p2=b