All Sky Radial Velocity Surveys using a Multi-Object Fixed Delay Interferometer

Suvrath Mahadevan, J. Ge, J. C. Van Eyken, C. DeWitt, S. Shaklan

Research output: Contribution to journalConference article

1 Citation (Scopus)

Abstract

Multi-object dispersed fixed-delay interferometry provides a powerful technique for all sky Doppler radial velocity (RV) searches for extrasolar planets. This technique takes advantage of the high sensitivity of a fixed-delay interferometer for precision Doppler RV measurements. The interferometer fringes are dispersed by a moderate resolution spectrometer for broad band observing. Compared to current state-of-the-art high resolution echelle techniques responsible for detection of more than 100 exoplanets, this technique offers several new capabilities such as wide field multiple object observation capability, high instrument throughput and stable instrument responses. The instrument can be used in the visible as well as in the near-IR and UV for observing stars with all spectral types from early A type to late M. Once this instrument is coupled with wide field telescopes (a few degrees of field of view, such as Sloan and WIYN), hundreds of stars with m v < 12 or brighter can be simultaneously monitored with Doppler precision of σ = 15 m/s or better within an hour integration. Millions of stars can be monitored annually. Thousands of extrasolar planets will be uncovered by this proposed all sky RV technique in a decade for studying planet formation and evolution. A prototype instrument has been used for observing at the KPNO 2.1m telescope in 2002, demonstrating a short term Doppler precision of ∼ 3 m/s with eta Gas (V = 3.5), a RV stable star. It also recovered the RV curve for 51 Peg (V = 5.5), confirming previous planet detection using the echelle spectrographs. The total measured detection efficiency from the above the atmosphere to the CCD detector is about 5% without iodine absorption under 1.5 arcsec seeing conditions, comparable to all of the echelle spectrometers for planet detection. A new instrument, fed with both interferometer outputs, is being developed with a higher efficiency Volume phase holographic grating and better optical design for an initial planet search at the KPNO 2.1m telescope in 2003. It will provide about 20% total detection efficiency. Details can be found in the companion paper in these proceedings. In this paper, we will present principle of the technique, and plans for all sky Doppler surveys for extrasolar planets.

Original languageEnglish (US)
Pages (from-to)184-192
Number of pages9
JournalProceedings of SPIE - The International Society for Optical Engineering
Volume5170
DOIs
StatePublished - Dec 1 2003
EventTechniques and Instrumentation for Detection of Exoplants - San Diego, CA, United States
Duration: Aug 5 2003Aug 7 2003

Fingerprint

Radial velocity
Interferometer
radial velocity
Interferometers
sky
Doppler
interferometers
Extrasolar planets
Planets
extrasolar planets
Extrasolar Planets
Echelle
Stars
Star
Telescopes
planet detection
Telescope
stars
Wide-field
telescopes

All Science Journal Classification (ASJC) codes

  • Electronic, Optical and Magnetic Materials
  • Condensed Matter Physics
  • Computer Science Applications
  • Applied Mathematics
  • Electrical and Electronic Engineering

Cite this

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title = "All Sky Radial Velocity Surveys using a Multi-Object Fixed Delay Interferometer",
abstract = "Multi-object dispersed fixed-delay interferometry provides a powerful technique for all sky Doppler radial velocity (RV) searches for extrasolar planets. This technique takes advantage of the high sensitivity of a fixed-delay interferometer for precision Doppler RV measurements. The interferometer fringes are dispersed by a moderate resolution spectrometer for broad band observing. Compared to current state-of-the-art high resolution echelle techniques responsible for detection of more than 100 exoplanets, this technique offers several new capabilities such as wide field multiple object observation capability, high instrument throughput and stable instrument responses. The instrument can be used in the visible as well as in the near-IR and UV for observing stars with all spectral types from early A type to late M. Once this instrument is coupled with wide field telescopes (a few degrees of field of view, such as Sloan and WIYN), hundreds of stars with m v < 12 or brighter can be simultaneously monitored with Doppler precision of σ = 15 m/s or better within an hour integration. Millions of stars can be monitored annually. Thousands of extrasolar planets will be uncovered by this proposed all sky RV technique in a decade for studying planet formation and evolution. A prototype instrument has been used for observing at the KPNO 2.1m telescope in 2002, demonstrating a short term Doppler precision of ∼ 3 m/s with eta Gas (V = 3.5), a RV stable star. It also recovered the RV curve for 51 Peg (V = 5.5), confirming previous planet detection using the echelle spectrographs. The total measured detection efficiency from the above the atmosphere to the CCD detector is about 5{\%} without iodine absorption under 1.5 arcsec seeing conditions, comparable to all of the echelle spectrometers for planet detection. A new instrument, fed with both interferometer outputs, is being developed with a higher efficiency Volume phase holographic grating and better optical design for an initial planet search at the KPNO 2.1m telescope in 2003. It will provide about 20{\%} total detection efficiency. Details can be found in the companion paper in these proceedings. In this paper, we will present principle of the technique, and plans for all sky Doppler surveys for extrasolar planets.",
author = "Suvrath Mahadevan and J. Ge and {Van Eyken}, {J. C.} and C. DeWitt and S. Shaklan",
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All Sky Radial Velocity Surveys using a Multi-Object Fixed Delay Interferometer. / Mahadevan, Suvrath; Ge, J.; Van Eyken, J. C.; DeWitt, C.; Shaklan, S.

In: Proceedings of SPIE - The International Society for Optical Engineering, Vol. 5170, 01.12.2003, p. 184-192.

Research output: Contribution to journalConference article

TY - JOUR

T1 - All Sky Radial Velocity Surveys using a Multi-Object Fixed Delay Interferometer

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N2 - Multi-object dispersed fixed-delay interferometry provides a powerful technique for all sky Doppler radial velocity (RV) searches for extrasolar planets. This technique takes advantage of the high sensitivity of a fixed-delay interferometer for precision Doppler RV measurements. The interferometer fringes are dispersed by a moderate resolution spectrometer for broad band observing. Compared to current state-of-the-art high resolution echelle techniques responsible for detection of more than 100 exoplanets, this technique offers several new capabilities such as wide field multiple object observation capability, high instrument throughput and stable instrument responses. The instrument can be used in the visible as well as in the near-IR and UV for observing stars with all spectral types from early A type to late M. Once this instrument is coupled with wide field telescopes (a few degrees of field of view, such as Sloan and WIYN), hundreds of stars with m v < 12 or brighter can be simultaneously monitored with Doppler precision of σ = 15 m/s or better within an hour integration. Millions of stars can be monitored annually. Thousands of extrasolar planets will be uncovered by this proposed all sky RV technique in a decade for studying planet formation and evolution. A prototype instrument has been used for observing at the KPNO 2.1m telescope in 2002, demonstrating a short term Doppler precision of ∼ 3 m/s with eta Gas (V = 3.5), a RV stable star. It also recovered the RV curve for 51 Peg (V = 5.5), confirming previous planet detection using the echelle spectrographs. The total measured detection efficiency from the above the atmosphere to the CCD detector is about 5% without iodine absorption under 1.5 arcsec seeing conditions, comparable to all of the echelle spectrometers for planet detection. A new instrument, fed with both interferometer outputs, is being developed with a higher efficiency Volume phase holographic grating and better optical design for an initial planet search at the KPNO 2.1m telescope in 2003. It will provide about 20% total detection efficiency. Details can be found in the companion paper in these proceedings. In this paper, we will present principle of the technique, and plans for all sky Doppler surveys for extrasolar planets.

AB - Multi-object dispersed fixed-delay interferometry provides a powerful technique for all sky Doppler radial velocity (RV) searches for extrasolar planets. This technique takes advantage of the high sensitivity of a fixed-delay interferometer for precision Doppler RV measurements. The interferometer fringes are dispersed by a moderate resolution spectrometer for broad band observing. Compared to current state-of-the-art high resolution echelle techniques responsible for detection of more than 100 exoplanets, this technique offers several new capabilities such as wide field multiple object observation capability, high instrument throughput and stable instrument responses. The instrument can be used in the visible as well as in the near-IR and UV for observing stars with all spectral types from early A type to late M. Once this instrument is coupled with wide field telescopes (a few degrees of field of view, such as Sloan and WIYN), hundreds of stars with m v < 12 or brighter can be simultaneously monitored with Doppler precision of σ = 15 m/s or better within an hour integration. Millions of stars can be monitored annually. Thousands of extrasolar planets will be uncovered by this proposed all sky RV technique in a decade for studying planet formation and evolution. A prototype instrument has been used for observing at the KPNO 2.1m telescope in 2002, demonstrating a short term Doppler precision of ∼ 3 m/s with eta Gas (V = 3.5), a RV stable star. It also recovered the RV curve for 51 Peg (V = 5.5), confirming previous planet detection using the echelle spectrographs. The total measured detection efficiency from the above the atmosphere to the CCD detector is about 5% without iodine absorption under 1.5 arcsec seeing conditions, comparable to all of the echelle spectrometers for planet detection. A new instrument, fed with both interferometer outputs, is being developed with a higher efficiency Volume phase holographic grating and better optical design for an initial planet search at the KPNO 2.1m telescope in 2003. It will provide about 20% total detection efficiency. Details can be found in the companion paper in these proceedings. In this paper, we will present principle of the technique, and plans for all sky Doppler surveys for extrasolar planets.

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