The Calan-Hertfordshire Extrasolar Planet Search

The Calan-Hertfordshire Extrasolar Planet Search

J.S. Jenkins 1Departamento de Astronomo, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago, Chile Casilla 36-D 1 jjenkins@das.uchile.cl    H.R.A. Jones 2Centre for Astrophysics, University of Hertfordshire, College Lane, Hatfield, Hertfordshire, AL10 9AB 2    K. Gozdziewski 3Torun Centre for Astronomy, Nicolaus Copernicus University, Gagarina 11, 87-100 Torun, Poland3    C. Migaszewski 3Torun Centre for Astronomy, Nicolaus Copernicus University, Gagarina 11, 87-100 Torun, Poland3    J.R. Barnes 2Centre for Astrophysics, University of Hertfordshire, College Lane, Hatfield, Hertfordshire, AL10 9AB 2    M.I. Jones 1Departamento de Astronomo, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago, Chile Casilla 36-D 1    P. Rojo 1Departamento de Astronomo, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago, Chile Casilla 36-D 1    D.J. Pinfield 2Centre for Astrophysics, University of Hertfordshire, College Lane, Hatfield, Hertfordshire, AL10 9AB 2    A.C. Day-Jones 1Departamento de Astronomo, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago, Chile Casilla 36-D 1    S. Hoyer 1Departamento de Astronomo, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago, Chile Casilla 36-D 1
Abstract

The detailed study of the exoplanetary systems HD189733 and HD209458 has given rise to a wealth of exciting information on the physics of exoplanetary atmospheres. To further our understanding of the make-up and processes within these atmospheres we require a larger sample of bright transiting planets. We have began a project to detect more bright transiting planets in the southern hemisphere by utilising precision radial-velocity measurements. We have observed a constrained sample of bright, inactive and metal-rich stars using the HARPS instrument and here we present the current status of this project, along with our first discoveries which include a brown dwarf/extreme-Jovian exoplanet found in the brown dwarf desert region around the star HD191760 and improved orbits for three other exoplanetary systems HD48265, HD143361 and HD154672. Finally, we briefly discuss the future of this project and the current prospects we have for discovering more bright transiting planets.

\session

-titleNew Technologies for Probing the Diversity of Brown Dwarfs and Exoplanets

1 Introduction

Since the discovery of the extrasolar planets (aka. exoplanets) 51 Pegasi  (Ref1 ) and 70 Virginis  (Ref2 ), arguably the most important exoplanetary discoveries were the detections of both HD209458  and HD189733 . These planets are the brightest transiting exoplanets known to date and both were first detected by radial-velocity variations (Ref3 , Ref4 ). Since these planets orbit bright stars, where radial-velocity samples are biased due to the required S/N levels needed for precision work, their transits have allowed follow-up from ground based and space based observatories. A number of pivotal discoveries have been made from these systems. For instance, Ref5 report the detection of both oxygen and carbon in the extended upper atmosphere of the planet orbiting HD209458  using STIS on the Hubble Space Telescope (HST) and Ref6 also used HST data to detect sodium absorption in the planet’s atmosphere. The mid infrared spectrum of the planet was measured by Ref7 using the Spitzer IRS instrument, indicating both thermal emission and a possible silicate cloud deck feature at 9.65m. However, follow-up from Ref8 has shown that the spectrum is dominated by thermal emission and there is no evidence in their data for the silicate feature reported by Ref7 . Also these data indicate possible heat redistribution between the planet’s dayside and nightside. In addition, the planet around HD189733 has also been extensively studied. The secondary eclipse has been measured (Ref9 ) and has revealed strong infrared emission from this planet. Ref10 claim the discovery of polarized light from this planet, representing the first such detection for any exoplanet. Also, a ground based transmission spectrum has revealed sodium absorption (Ref11 ), using the Hobby-Eberly Telescope to observe the planet across 11 orbits, and the level was found to be three times larger than that previously found for HD209458  (Ref6 ). Both Ref12 and Ref13 have used the HST NICMOS spectrograph to measure water absorption and methane absorption in the atmosphere of HD187933 , along with other molecular bands such as carbon monoxide and carbon dioxide, which are the first detections of carbon based molecules in any exoplanet. These observations now allow one to compare the atmospheric properties of extrasolar planets and also to test numerous model atmospheres (e.g. Ref14 , Ref15 , Ref16 ).

2 The Calan-Hertfordshire Extrasolar Planet Search

From the list of detailed studies shown above, it is clear that a larger census of transiting planets around bright stars will provide the exoplanetary community with a database that can be used to examine a wider range of properties that constitute the atmospheres of exoplanets. This particularly holds true in the southern hemisphere where no really bright transiting planets yet exist and where some of the worlds leading telescopes and instrumentation (e.g. the VLT) lie in wait to examine such systems. Therefore, we have began a targeted project in the southern hemisphere that aims to detect more 51 Peg -like planets and hence more bright transiting exoplanets. The Calan-Hertfordshire Extrasolar Planet Search (aka. CHEPS) utilises the radial-velocity technique to monitor a number of bright, inactive and metal-rich, solar-type stars to hunt for the typical high frequency radial-velocity amplitude induced by an orbiting short period world.

The current CHEPS target list is drawn from an initial southern sample of 350 stars that were observed with the ESO-FEROS spectrograph (Ref17 ). The results from the analysis of this initial sample were published in Ref18 . In brief, these stars were all pre-selected from the Hipparcos catalogue to have colours in the range 0.50.9 and magnitudes in the range 7.59.5. This helps to select solar-type stars that are not on any previous planet search list (i.e. essentially all Sun-like stars brighter than 7.5 in already constitute other planet search target lists) but the stars are bright enough that a detected transiting planet, exhibiting a fairly deep transit light curve, will attain benchmark status and provide an ideal target for atmospheric follow-up studies. The FEROS chromospheric activities were then measured following the prescription explained in (Ref19 ) to extract each star’s log-index, which can be used as a proxy for the expected level of radial-velocity jitter (e.g. Ref20 ). All stars with log -4.5 were included in the CHEPS target list, with the highest priority given to those stars closer to solar activity levels or less (i.e. -4.9). In addition to the activity criteria we also aim to increase the probability of gas giant planet detection by measuring the metallicity, or iron abundance ([Fe/H]) of each of our possible planet search targets, since Ref22 have shown that the probability of gas giant planet detection increases exponentially with the amount of iron found in the photospheres of solar-type stars. This result can be explained in the framework of giant planet formation through core accretion of gas depleted materials left over from the formation of the parent star (e.g. Ref24 ). Therefore, we only consider stars with a FEROS iron abundance ratio +0.1 dex for our planet search project, which should help to bias the sample towards more gas giant-like exoplanets. In all, 100 stars were drawn from this pilot sample and almost all have been followed up with HARPS to hunt for short period planets.

Thus far the CHEPS has obtained at least three radial-velocity points for over 95% of this pilot sample using the ESO-HARPS instrument (Ref25 ). Of these stars, a total of over 25 significant radial-velocity variations have been detected (after ruling out spectroscopic binary companions) giving rise to a high fraction of planet like signals (25%). In Ref27 we present the first results from this data, announcing the discovery of a brown dwarf/extreme-Jovian exoplanet located in the brown dwarf desert region around the star HD191760 (Fig. 1). The likelihood is that this companion is a sub-stellar brown dwarf yet the possibility exists that it is actually a deuterium burning extreme-Jovian exoplanet that formed through core accretion. Theoretically such companions are possible up to masses of around 40M orbiting solar-type stars with super-solar metallicities and are likely to be found within the brown dwarf desert region at semimajor axes of 1-4 AU (Ref28 ,Ref30 ). Panel (a) shows all the data obtained for this star (red filled points) performing a bisector velocity span (BVS) correction (see Ref31 for details). The solid blue curve reveals a companion with a period of 505.650.42 days, a M sin  of 38.171.02M and a fairly eccentric orbit of 0.630.01. All orbital parameters are listed in Ref27 . Panels (b) and (c) show the residuals of the best fits to the data before and after the BVS correction respectively. Clearly by measuring the BVS and using it to clean the radial-velocity points from any line broadening effects such as stellar activity (panels d and e), a much improved solution can be extracted. Also, we ran extensive GAMP stability simulations (Ref32 ) to hunt for regions where additional planetary mass companions could reside in the system. From this analysis we found that all regions beyond 0.17 AU and out as far as the detected companion are chaotic, due to the disastrous gravity imposed by this massive companion along its eccentric orbit, and therefore if any additional companions reside in the systems within the orbit of this detected companion they are likely very low-mass, short period bodies.

Figure 1: Panel (a) shows the best fit Keplerian solution to the Dopper points for HD191760 with BVS correction as in Ref31 . Panel (b) shows the residuals without BVS correction and panel (c) shows the residuals after correction, corresponding to the synthetic curve in panel (a). Panel (d) shows the radial-velocities against the BVS after subtraction of the best-fitting Keplerian synthetic curve. Panel (e) shows the best-fitting linear correlation coefficient of BVS-RV. Note that the two values with the largest BVS help to better constrain the correlation.

Along with this interesting discovery, we also show updated orbits for three exoplanets recently announced from the Magellan Planet Search (Fig. 2). The left panel shows the best fit to the star HD48265, the middle panel is for HD143361 and the right panel shows the fit to the data for HD154672, all using the Systemic fitting tool (Ref33 ). The blue data points represent the values published by the Magellan Planet Search (Ref34 , Ref35 ) and the green data are those from our work. The updated orbits for these systems are listed in Ref27 and due to the pre-selection of the target list to focus on the most inactive targets, the rms residuals for three of these systems is only 2-3ms. HD48265 presents a larger rms scatter due to one errant Magellan data point that has larger residuals than the other points and when removed the rms drops to almost 3ms. All three of these planets are found to have minimum masses that would place them in the gas giant regime and none are found to have very short periods. Note that at present we do not find any significant evidence for additional planets in any of these systems.

Although we initially predicted a yield of 12 planets, as mentioned above, we currently show over 25 planetary-like signals in the pilot sample. This is because the Ref22 relation is only complete for gas giant planets down to minimum masses of 0.4M and with amplitudes () of 30ms, whereas within our planet-like signals we have a number of potential lower mass systems across a wide range of periods. Such systems require both time and data to properly confirm and constrain.

Figure 2: The radial-velocity Keplerian fits to the stars HD48265 (left), HD143361 (middle) and HD154672 (right). Plotted in blue are the literature values from the Magellan program and in green are the data points from Ref27 .

3 Summary and Future Work

We briefly discuss recent results from the Calan-Hertfordshire Extrasolar Planet Search (CHEPS) that reveal 1) the discovery of a brown dwarf/extreme-Jovian exoplanet in the brown dwarf desert region around the star HD191760 and 2) updated orbits for three recently discovered exoplanets (HD48265 , HD143361  and HD154672 ). The CHEPS project is currently ongoing and with future time already awarded we expect to announce many more exoplanets around these stars, in addition to more transiting planets that can be followed up from the ground and space to probe the physics of exoplanetary atmospheres. Finally, we have significantly increased the target sample from the initial 100 pilot stars that were drawn from the 350 stars analysed using FEROS. We observed a further 500 stars with FEROS and have recently measured their activities and metallicities, giving rise to a three-fold increase in the number of inactive and metal-rich targets we can follow up to hunt for more southern short period exoplanets.

References

  • (1) Mayor & Queloz, Nature 378, (1995) 355
  • (2) Marcy & Butler, ApJ, 464, (1996) 147
  • (3) Henry et al., ApJL 529, (1999) L41
  • (4) Bouchy et al., A&A 444, (2005) L15
  • (5) Vidal-Madjar et al., ApJ 604, (2004) 69
  • (6) Charbonneau et al., ApJ 568, (2002) 377
  • (7) Richardson et al., Nature 445 (2007) 892
  • (8) Swain et al., ApJ 674, (2008) 482
  • (9) Deming et al., ApJ 644, (2006) 560
  • (10) Berdyugina et al., ApJ 673, (2008) 83
  • (11) Redfield et al., ApJ 673, (2008) 87
  • (12) Swain et al., Nature 452, (2008) 329
  • (13) Swain et al. ApJL 690, (2009) 114
  • (14) Baraffe et al., A&A 402, (2003) 701
  • (15) Burrows et al., ApJ 678, (2008) 1436
  • (16) Fortney et al., ApJ 678, (2008) 1419
  • (17) Kaufer et al., The Messenger 95, (1999) 8
  • (18) Jenkins et al., A&A 485, (2008) 571
  • (19) Noyes et al., ApJ 279, (1984) 763
  • (20) Saar, Butler & Marcy, ApJL 498, (1998) L15
  • (21) Fischer & Valenti, ApJ 622, (2005) 1102
  • (22) Alibert et al., A&A 434, (2005) 343
  • (23) Mayor et al., The Messenger 114, (2003) 20
  • (24) Jenkins et al., MNRAS 398, (2009) 911
  • (25) Baraffe, Chabrier & Barman, A&A 482, (2008) 315
  • (26) Mordasini et al., A&A 501, (2009b) 1161
  • (27) Migaszewski & Nowak, Conf. Proc. arxiv:0901.0202, (2009)
  • (28) Gozdziewski & Konacki, ApJ 647, (2006) 573
  • (29) Meschiari et al., PASP 121, (2009) 1016
  • (30) Lopez-Morales et al., AJ 136, (2008) 1901
  • (31) Minniti et al., ApJ 693, (2009) 1424
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
295998
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description