The planet search program at the ESO Coudé Echelle spectrometer

Endl, Michael; Kürster, M.; Els, S.; Hatzes, A. P.; Cochran, William D.; Dennerl, K.; Döbereiner, S.

doi:10.1051/0004-6361:20020937

Cited by 74 publications

(103 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…τ Cet has the smallest variations in log R HK in the sample. κ For: the RVs of κ For decline over the whole time baseline of 14 yr which indicates an orbital period longer than the estimate of 21 yr given in Endl et al (2002). The Keplerian period of 10 700 d listed in Table 4 (29.3 yr) is not well constrained.…”

Section: Discussion On Individual Targetsmentioning

confidence: 80%

“…An iodine gas absorption cell provided the wavelength calibration. More details about the instrument, data analysis, as well as the obtained results can be found in Endl et al (2002). Table 3 lists the radial velocity results.…”

Section: Ces + Long Cameramentioning

confidence: 99%

“…To limit the light from adjacent wavelength regions a set of filters were applied: a coloured glass filter type VG11, a notch-filter to reduce the internal laser light, and a hot mirror to suppress the red spectrum. While the iodine cell laboratory spectrum previously used by Endl et al (2002) in their analysis of the CES+LC data had only R = 400 000, the new scan ensures an iodine spectrum with a resolution almost 5 times higher than the resolution of the CES+VLC.…”

Section: Ces + Very Long Cameramentioning

confidence: 99%

“…the same wavelength calibrator. Because Endl et al (2002) calculated the LC RVs with different stellar templates and an iodine spectrum of lower resolution than used in this work, we re-calculated the RVs for all LC spectra with the same VLC stellar template (which is shorter than the LC spectra) and the new iodine cell scan to have the same reference for the LC and VLC. The re-calculated RVs are verified to have a precision similar to the published LC data.…”

Section: Combining the Lc And Vlc Datamentioning

confidence: 99%

“…We corrected all re-calculated LC RVs for this systematic offset. Finally, we adjusted the RV mean of the published LC time series (Endl et al 2002) to fit the RV mean of the re-calculated time series. In Figs. 19-23 the LC (Endl et al 2002) and VLC data are always shown relative to each other with the measured and corrected offset (and not with a fitted RV offsets that could have been taken from our fit results presented below in Sect.…”

Section: Combining the Lc And Vlc Datamentioning

confidence: 99%

See 4 more Smart Citations

The planet search programme at the ESO CES and HARPS

Zechmeister

Kürster

Endl³

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

Context. In 1992 we began a precision radial velocity survey for planets around solar-like stars with the Coudé Echelle Spectrograph and the Long Camera (CES LC) at the 1.4 m telescope in La Silla (Chile) resulting in the discovery of the planet ι Hor b. We have continued the survey with the upgraded CES Very Long Camera (VLC) and the HARPS spectrographs, both at the 3.6 m telescope, until 2007. Aims. In this paper we present additional radial velocities for 31 stars of the original sample with higher precision. The observations cover a time span of up to 15 years and permit a search for Jupiter analogues. Methods. The survey was carried out with three different instruments/instrument configurations using the iodine absorption cell and the ThAr methods for wavelength calibration. We combine the data sets and perform a joint analysis for variability, trends, and periodicities. We compute Keplerian orbits for companions and detection limits in case of non-detections. Moreover, the HARPS radial velocities are analysed for correlations with activity indicators (CaII H&K and cross-correlation function shape). Results. We achieve a long-term RV precision of 15 m/s (CES+LC, 1992-1998, 9 m/s (CES+VLC, 1999, and 2.8 m/s (HARPS, 2003(HARPS, -2009, including archive data), respectively. This enables us to confirm the known planetary signals in ι Hor and HR 506 as well as the three known planets around HR 3259. A steady RV trend for Ind A can be explained by a planetary companion and calls for direct imaging campaigns. On the other hand, we find previously reported trends to be smaller for β Hyi and not present for α Men. The candidate planet Eri b was not detected despite our better precision. Also the planet announced for HR 4523 cannot be confirmed. Long-term trends in several of our stars are compatible with known stellar companions. We provide a spectroscopic orbital solution for the binary HR 2400 and refined solutions for the planets around HR 506 and ι Hor. For some other stars the variations could be attributed to stellar activity, as e.g. the magnetic cycle in the case of HR 8323. Conclusions. The occurrence of two Jupiter-mass planets in our sample is in line with the estimate of 10% for the frequency of giant planets with periods smaller than 10 yr around solar-like stars. We have not detected a Jupiter analogue, while the detections limits for circular orbits indicate at 5 AU a sensitivity for minimum mass of at least 1M Jup (2M Jup ) for 13% (61%) of the stars.

show abstract

Section: Discussion On Individual Targetsmentioning

confidence: 80%

Section: Ces + Long Cameramentioning

confidence: 99%

Section: Ces + Very Long Cameramentioning

confidence: 99%

Section: Combining the Lc And Vlc Datamentioning

confidence: 99%

Section: Combining the Lc And Vlc Datamentioning

confidence: 99%

See 3 more Smart Citations

The planet search programme at the ESO CES and HARPS

Zechmeister

Kürster

Endl³

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

Radial velocities from automated telescopes

Pepe

Mayor

2004

Astron Nachr

View full text Add to dashboard Cite

Abstract. During the past years, precise radial-velocity measurements have been the fundamental tool for the discovery and characterization of almost all the presently known extra-solar planets. The increasing precision and efficiency of this technique has also opened new possibilities for the follow-up of planetary transit candidates, as well as for other fields of astronomy, such as asteroseismology and stellar physics. The example of extra-solar planets illustrates quite clearly the strong need for large observational surveys: 1) In order to get a complete view of the planet "zoo", many stars of various types must be measured and followed up.2) The detection efficiency increases enormously with the quality and the quantity of data points. Time sampling is a critical parameter.3) The great diversity of known planetary systems requires covering observation time-scales from one night to several years and even decades. A direct consequence of these factors is that survey programmes require a large amount of telescope time and a continuous follow-up of the observations. In a context of limited resources and large amounts of data, automated telescopes will be of great help, or even required, to carry out these programmes. Based on our experience with CORALIE and HARPS, we shall try to define a series of "requirements" towards automated telescopes for precise radial-velocity measurements.

show abstract

The Mt John University Observatory search for Earth-mass planets in the habitable zone of α Centauri

Endl

Bergmann

Hearnshaw

et al. 2014

International Journal of Astrobiology

View full text Add to dashboard Cite

The 'holy grail' in planet hunting is the detection of an Earth-analogue: a planet with similar mass as the Earth and an orbit inside the habitable zone. If we can find such an Earth-analogue around one of the stars in the immediate solar neighbourhood, we could potentially even study it in such great detail to address the question of its potential habitability. Several groups have focused their planet detection efforts on the nearest stars. Our team is currently performing an intensive observing campaign on the α Centauri system using the High Efficiency and Resolution Canterbury University Large Échelle Spectrograph (HERCULES) at the 1 m McLellan telescope at Mt John University Observatory in New Zealand. The goal of our project is to obtain such a large number of radial velocity (RV) measurements with sufficiently high temporal sampling to become sensitive to signals of Earth-mass planets in the habitable zones of the two stars in this binary system. Over the past few years, we have collected more than 45 000 spectra for both stars combined. These data are currently processed by an advanced version of our RV reduction pipeline, which eliminates the effect of spectral cross-contamination. Here we present simulations of the expected detection sensitivity to low-mass planets in the habitable zone by the HERCULES programme for various noise levels. We also discuss our expected sensitivity to the purported Earth-mass planet in a 3.24-day orbit announced by Dumusque et al. (2012).

show abstract

The planet search program at the ESO Coudé Echelle spectrometer

Cited by 74 publications

References 38 publications

The planet search programme at the ESO CES and HARPS

The planet search programme at the ESO CES and HARPS

Radial velocities from automated telescopes

The Mt John University Observatory search for Earth-mass planets in the habitable zone of α Centauri

Contact Info

Product

Resources

About