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| [[Image:orbit3.gif|thumb|right|200px|Diagram showing how a smaller object (such as an [[extrasolar planet]]) orbiting a larger object (such as a [[star]]) could produce changes in position and velocity of the latter as they orbit their common [[center of mass]] (red cross).]]
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| [[File:ESO - The Radial Velocity Method (by).jpg|thumb|right|Doppler spectroscopy detects periodic shifts in radial velocity by recording variations in the color of light from the host star. When a star moves towards Earth, its spectrum is blueshifted, while it is redshifted when it moves away from us. By analyzing these spectral shifts, astronomers can deduce the gravitational influence of extrasolar planets.]]
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| '''Doppler spectroscopy''' (also known as the '''radial-velocity method''', or colloquially, the '''wobble method''') is an [[Methods of detecting extrasolar planets|indirect method]] for finding [[extrasolar planet]]s and [[brown dwarf]]s from [[radial velocity|radial-velocity]] measurements via observation of [[Doppler shift]]s in the [[spectrum]] of the [[planet|planet's]] parent star.
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| About half of the extrasolar planets known were discovered using Doppler spectroscopy, as of October 2012.<ref name="Encyclopaedia">{{cite web |last1=Schneider |first1=Jean |date=26 October 2012 |title=Interactive Extra-solar Planets Catalog |url=http://exoplanet.eu/catalog.php |work=[[The Extrasolar Planets Encyclopedia]] |accessdate=2012-10-26}}</ref>
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| == History ==
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| [[File:Exoplanet Discovery Method Bar RV.png|thumb|250px|Exoplanets discovered by year (as of October 11, 2013). Those discovered using radial velocity are shown in black, whilst all other methods are in light grey.]]
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| [[Image:Doppler Shift vs Time.jpg|frame]]
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| [[Image:51 Peg b rv.jpg|thumb|right|275px|The method in action: the radial-velocity trend of 51 Pegasi indicates the presence of an unseen companion. The gravitational influence of the planet on the star is measured at ~56 m/s, with an orbital period of just 4.2 Earth days.]]
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| [[Image:Exoplanet Period-Mass Scatter Discovery Method RV.png|thumb|250px|right|Properties (mass and semimajor axis) of planets discovered through 2013 using radial velocity, compared (light gray) with planets discovered using other methods.]]
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| [[Otto Struve]] proposed in 1952 the use of powerful [[spectrograph]]s to detect distant planets. He described how a very large planet, as large as [[Jupiter]], for example, would cause its parent star to wobble slightly as the two objects orbit around their center of mass.<ref name="OBSERV">
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| {{cite journal
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| |author=[[Otto Struve|O. Struve]]
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| |title=Proposal for a project of high-precision stellar radial velocity work
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| |journal=[[The Observatory (journal)|The Observatory]]
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| |volume=72 |issue=870 |pages=199–200
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| |year=1952
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| |bibcode=1952Obs....72..199S
| |
| }}</ref> He predicted that the small Doppler shifts to the light emitted by the star, caused by its continuously varying radial velocity, would be detectable by the most sensitive spectrographs as tiny [[red shift]]s and [[blue shift]]s in the star's emission. However, the technology of the time produced radial-velocity measurements with errors of 1,000 [[m/s]] or more, making them useless for the detection of orbiting planets.<ref name="RVM">
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| {{cite web
| |
| |title=Radial velocity method
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| |url=http://www.daviddarling.info/encyclopedia/R/radial_velocity_method.html
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| |publisher=The Internet Encyclopedia of Science
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| |accessdate=2007-04-27
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| }}</ref> The expected changes in radial velocity are very small – Jupiter causes the [[Sun]] to change velocity by about 12.4 m/s over a period of 12 years, and the [[Earth]]'s effect is only 0.1 m/s over a period of 1 year – so long-term observations by instruments with a very high [[Optical resolution|resolution]] are required.<ref name="RVM"/><ref name="Wolszczan">
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| {{cite web
| |
| |author=[[Alex Wolszczan|A. Wolszczan]]
| |
| |title=Doppler spectroscopy and astrometry – Theory and practice of planetary orbit measurements
| |
| |url=http://www.astro.psu.edu/users/alex/astro497_2.pdf |format=PDF
| |
| |work=[http://www.astro.psu.edu/users/alex/Teaching_spring06.html ASTRO 497: "Astronomy of Extrasolar Planets" lectures notes]
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| |publisher=[[Penn State University]]
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| |date=Spring 2006
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| |accessdate=2009-04-19
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| }}</ref>
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| | |
| Advances in spectrometer technology and observational techniques in the 1980s and 1990s produced instruments capable of detecting the first of many new extrasolar planets. The [[ELODIE spectrograph]], installed at the [[Haute-Provence Observatory]] in Southern France in 1993, could measure radial-velocity shifts as low as 7 m/s, low enough for an extraterrestrial observer to detect Jupiter's influence on the Sun.<ref name = "ELODIE">{{cite web
| |
| | title= A user's guide to Elodie archive data products
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| | url = http://www.obs-hp.fr/www/archive/elodie-for-dummies.html
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| | publisher = Haute-Provence Observatory
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| | date = May 2009
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| | accessdate = 26 October 2012}}</ref> Using this instrument, astronomers [[Michel Mayor]] and [[Didier Queloz]] identified [[51 Pegasi b]], a "[[Hot Jupiter]]" in the constellation Pegasus.<ref name = "Nature">{{cite journal | url= | author=Mayor, Michael; Queloz, Didier | title=A Jupiter-mass companion to a solar-type star | journal=[[Nature (journal)|Nature]] | volume=378 |issue=6555 |year=1995 | pages=355–359| doi=10.1038/378355a0| format= | bibcode=1995Natur.378..355M}}</ref> Although planets had previously been detected orbiting [[pulsars]], 51 Pegasi b was the first planet ever found orbiting a [[main-sequence]] star, and the first detected using Doppler spectroscopy.
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| In November 1995, the scientists published their findings in the journal [[Nature (journal)|''Nature'']]; the paper has since been cited over 1,000 times. Since that date, over 700 exoplanet candidates have been identified, and most have been detected by Doppler search programs based at the [[Keck Observatory|Keck]], [[Lick Observatory|Lick]], and [[Anglo-Australian Observatory|Anglo-Australian]] Observatories (respectively, the California, Carnegie and Anglo-Australian planet searches), and teams based at the [[Geneva Extrasolar Planet Search]].<ref name="CNE">{{cite journal
| |
| |author=[[R. Paul Butler|R.P. Butler]] ''et al''.
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| |title=Catalog of Nearby Exoplanets
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| |url=http://exoplanets.org/cne.pdf |format=PDF
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| |journal=[[Astrophysical Journal]]
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| |volume=646 |issue=2–3 |pages=25–33
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| |year=2006
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| }}</ref>
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| Beginning in the early 2000s, a second generation of planet-hunting spectrographs permitted far more precise measurements. The [[HARPS]] spectrograph, installed at the [[La Silla Observatory]] in [[Chile]] in 2003, can identify radial-velocity shifts as small as 0.3 m/s, enough to locate many rocky, Earth-like planets.<ref name="HARPS">{{cite journal
| |
| | title=Setting New Standards With HARPS
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| | url=http://www.eso.org/sci/facilities/lasilla/instruments/harps/science/papers/harps_mess114.pdf
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| | author=Mayor ''et al.''
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| | journal=ESO Messenger
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| | volume=114
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| | pages=20
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| | year=2003}}</ref> A third generation of spectrographs is expected to come online in 2017. With measurement errors estimated below 0.1 m/s, these new instruments would allow an extraterrestrial observer to detect even Earth.<ref name = "ESPRESSO">{{cite web |url=http://espresso.astro.up.pt/ |title=ESPRESSO - Searching for other Worlds |date=2009-12-16 |publisher=Centro de Astrofísica da Universidade do Porto |accessdate=2010-10-26}}</ref>
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| == Procedure ==
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| A series of observations is made of the spectrum of light emitted by a star. Periodic variations in the star's spectrum may be detected, with the [[wavelength]] of characteristic [[spectral line]]s in the spectrum increasing and decreasing regularly over a period of time. Statistical filters are then applied to the data set to cancel out spectrum effects from other sources. Using mathematical [[best-fit]] techniques, astronomers can isolate the tell-tale periodic [[sine wave]] that indicates a planet in orbit.<ref name = "Nature"/>
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| If an extrasolar planet is detected, a [[minimum mass]] for the planet can be determined from the changes in the star's radial velocity. To find a more precise measure of the mass requires knowledge of the inclination of the planet's orbit. A graph of measured radial velocity versus time will give a characteristic curve ([[sine curve]] in the case of a circular orbit), and the amplitude of the curve will allow the minimum mass of the planet to be calculated.
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| The Bayesian Kepler periodogram is a mathematical [[algorithm]], used to detect single or multiple extrasolar planets from successive [[radial velocity|radial-velocity]] measurements of the star they are orbiting. It involves a [[Bayesian statistical analysis]] of the radial-velocity data, using a [[Prior probability|prior]] [[probability distribution]] over the space determined by one or more sets of Keplerian orbital parameters. This analysis may be implemented using the [[Markov chain]] [[Monte Carlo method|Monte Carlo]] (MCMC) method.
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| The method has been applied to the [[HD 208487]] system, resulting in an apparent detection of a second planet with a period of approximately 1000 days. However, this may be an artifact of stellar activity.<ref>
| |
| {{cite journal
| |
| |author=P.C. Gregory
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| |title=A Bayesian Kepler periodogram detects a second planet in HD 208487
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| |journal=Monthly Notices of the Royal Astronomical Society
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| |volume=374 |issue=4 |pages=1321–1333
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| |year=2007
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| |doi=10.1111/j.1365-2966.2006.11240.x
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| |bibcode=2007MNRAS.374.1321G
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| |arxiv = astro-ph/0609229 }}</ref><ref>
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| {{cite journal
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| |url=http://www.iop.org/EJ/article/0004-637X/657/1/533/65907.html
| |
| |author=Wright ''et al.''
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| |title=Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars
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| |journal=[[The Astrophysical Journal]]
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| |volume=657 | issue=1 | pages=533–545
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| |year=2007
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| |doi=10.1086/510553
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| |bibcode=2007ApJ...657..533W
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| |last2=Marcy
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| |first2=G. W.
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| |last3=Fischer
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| |first3=D. A
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| |last4=Butler
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| |first4=R. P.
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| |last5=Vogt
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| |first5=S. S.
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| |last6=Tinney
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| |first6=C. G.
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| |last7=Jones
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| |first7=H. R. A.
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| |last8=Carter
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| |first8=B. D.
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| |last9=Johnson
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| |first9=J. A.
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| |arxiv = astro-ph/0611658 }}</ref> The method is also applied to the [[HD 11964]] system, where it found an apparent planet with a period of approximately 1 year. However, this planet was not found in re-reduced data,<ref>
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| {{cite journal
| |
| |author=P.C. Gregory
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| |title=A Bayesian periodogram finds evidence for three planets in HD 11964
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| |journal=[[Monthly Notices of the Royal Astronomical Society]]
| |
| |volume=381 |issue=4 |pages=1607–1616
| |
| |year=2007
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| |doi=10.1111/j.1365-2966.2007.12361.x
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| |bibcode=2007MNRAS.381.1607G
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| |arxiv = 0709.0970 }}</ref><ref>
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| {{cite journal
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| |author=J.T. Wright ''et al.''
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| |title=Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems
| |
| |year=2008
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| |doi=10.1088/0004-637X/693/2/1084
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| |journal=The Astrophysical Journal
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| |volume=693
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| |issue=2
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| |pages=1084–1099
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| |arxiv=0812.1582
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| |bibcode = 2009ApJ...693.1084W }}</ref> suggesting that this detection was an artifact of the Earth's orbital motion around the Sun.{{citation needed|date=March 2010}}
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| Although radial-velocity of the star only gives a planet's minimum mass, if the planet's [[spectral line]]s can be distinguished from the star's spectral lines then the radial-velocity of the planet itself can be found and this gives the inclination of the planet's orbit and therefore the planet's actual mass can be determined. The first non-transiting planet to have its mass found this way was [[Tau Boötis b]] in 2012 when [[carbon monoxide]] was detected in the infra-red part of the spectrum.<ref>[http://arxiv.org/abs/1206.6197 Weighing The Non-Transiting Hot Jupiter Tau BOO b], Florian Rodler, Mercedes Lopez-Morales, Ignasi Ribas, 27 June 2012</ref>
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| === Example ===
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| The graph to the right illustrates the [[sine curve]] created using Doppler spectroscopy to observe the radial velocity of an imaginary star which is being orbited by a planet in a circular orbit. Observations of a real star would produce a similar graph, although [[Orbital eccentricity|eccentricity]] in the orbit will distort the curve and complicate the calculations below.
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| This theoretical star's velocity shows a periodic variance of ±1 m/s, suggesting an orbiting mass that is creating a gravitational pull on this star. Using [[Kepler]]'s [[Kepler's laws of planetary motion|third law of planetary motion]], the observed period of the planet's orbit around the star (equal to the period of the observed variations in the star's spectrum) can be used to determine the planet's distance from the star (<math>r</math>) using the following equation:
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| <math>r^3=\frac{GM_{star}}{4\pi^2}P_{star}^2\,</math>
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| where:
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| *''r'' is the distance of the planet from the star
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| *''G'' is the [[gravitational constant]]
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| *''M<sub>star</sub>'' is the mass of the star <!-- how is this determined?-->
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| *''P<sub>star</sub>'' is the observed period of the star
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| Having determined <math>r</math>, the velocity of the planet around the star can be calculated using [[Isaac Newton|Newton]]'s [[law of gravitation]], and the [[orbit equation]]:
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| <math>V_{PL}=\sqrt{GM_{star}/r}\,</math>
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| where <math>V_{PL}</math> is the velocity of planet.
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| The mass of the planet can then be found from the calculated velocity of the planet:
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| <math>M_{PL}=\frac{M_{star}V_{star}}{V_{PL}}\,</math>
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| where <math>V_{star}</math> is the velocity of parent star. The observed Doppler velocity, <math>K = V_{star}\sin(i)</math>, where ''i'' is the [[inclination]] of the planet's orbit to the line perpendicular to the [[Line-of-sight propagation|line-of-sight]].
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| Thus, assuming a value for the inclination of the planet's orbit and for the mass of the star, the observed changes in the radial velocity of the star can be used to calculate the mass of the extrasolar planet.
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| ==Radial-velocity comparison tables==
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| {| class="wikitable"
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| |+
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| ![[Planet]] [[Mass]]
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| !Distance <br>[[Astronomical Unit|AU]]
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| !Radial velocity <br>(''v''<sub>radial</sub>)
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| !Notice
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| |-
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| | [[Jupiter]]
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| | 1
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| | 28.4 [[Metre|m]]/[[Second|s]]
| |
| |
| |
| |-
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| | [[Jupiter]]
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| | 5
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| | 12.7 m/s
| |
| |
| |
| |-
| |
| | [[Neptune]]
| |
| | 0.1
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| | 4.8 m/s
| |
| |
| |
| |-
| |
| | [[Neptune]]
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| | 1
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| | 1.5 m/s
| |
| |
| |
| |-
| |
| | [[Super-Earth]] (5 M⊕)
| |
| | 0.1
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| | 1.4 m/s
| |
| |
| |
| |-
| |
| | [[Alpha Centauri Bb]] (1.13 ± 0.09 M⊕)
| |
| | 0.04
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| | 0.51 m/s
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| | (1<ref name="eso1">{{cite web|url=http://www.eso.org/public/news/eso1241/ |title=Planet Found in Nearest Star System to Earth |publisher=[[European Southern Observatory]] |date=16 October 2012 |accessdate=17 October 2012}}</ref>)
| |
| |-
| |
| | [[Super-Earth]] (5 M⊕)
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| | 1
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| | 0.45 m/s
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| |
| |
| |-
| |
| | [[Earth]]
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| | 1
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| | 0.09 m/s
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| |
| |
| |}
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| Ref:<ref name="Chinese Academy of Sciences">{{cite web |url=http://202.127.29.4/bdep_meeting/download/talks/20July/10-LPasquini.ppt |title= ESPRESSO and CODEX the next generation of RV planet hunters at ESO |date=2010-10-16 |publisher=[[Chinese Academy of Sciences]] |accessdate=2010-10-16}}</ref>
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| Notice 1: Most precise ''v''<sub>radial</sub> measurements ever recorded. [[European Southern Observatory|ESO]]'s [[HARPS]] spectrograph was used.<ref name="eso1" />
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| <div style="float:left">
| |
| {| class="wikitable"
| |
| |+ Planets<ref name="Chinese Academy of Sciences"/>
| |
| ! Planet
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| ! Planet Type <br>
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| !Semimajor Axis <br>([[Astronomical unit|AU]])
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| !Orbital Period <br>
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| ![[Radial velocity]]<br>(m/s)
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| ! Detectable by:
| |
| |-
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| | [[51 Pegasi b]]
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| | [[Hot Jupiter]]
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| | 0.05
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| | 4.23 days
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| | 55.9<ref>{{cite web
| |
| | url = http://exoplanets.org/detail/51_Peg_b
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| | publisher = Exoplanets Data Explorer
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| | title = 51 Peg b
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| }}</ref>
| |
| | First-generation spectrograph
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| |-
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| | [[55 Cancri d]]
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| | [[Gas giant]]
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| | 5.77
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| | 14.29 years
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| | 45.2<ref>{{cite web
| |
| | url = http://exoplanets.org/detail/55_Cnc_d
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| | publisher = Exoplanets Data Explorer
| |
| | title = 55 Cnc d
| |
| }}</ref>
| |
| | First-generation spectrograph
| |
| |-
| |
| | [[Jupiter]]
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| | [[Gas giant]]
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| | 5.20
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| | 11.86 years
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| | 12.4<ref name = "Texas">{{cite web
| |
| | url = http://austral.as.utexas.edu/michael/teaching/AST_s309_ss11_2.ppt
| |
| | last = Endl
| |
| | first = Michael
| |
| | title = The Doppler Method, or Radial Velocity Detection of Planets
| |
| | publisher = University of Texas at Austin
| |
| | accessdate = 26 October 2012
| |
| }}</ref>
| |
| | First-generation spectrograph
| |
| |-
| |
| | [[Gliese 581c]]
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| | [[Super-Earth]]
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| | 0.07
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| | 12.92 days
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| | 3.18<ref>{{cite web
| |
| | url = http://exoplanets.org/detail/GJ_581_c
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| | publisher = Exoplanets Data Explorer
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| | title = GJ 581 c
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| }}</ref>
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| | Second-generation spectrograph
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| |-
| |
| |-
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| | [[Saturn]]
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| | [[Gas giant]]
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| | 9.58
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| | 29.46 years
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| | 2.75
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| | Second-generation spectrograph
| |
| |-
| |
| | [[Alpha Centauri Bb]]
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| | [[Terrestrial planet]]
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| | 0.04
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| | 3.23 days
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| | 0.510<ref>{{cite web
| |
| | url = http://exoplanets.org/detail/alpha_Cen_B_b
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| | publisher = Exoplanets Data Explorer
| |
| | title = alpha Cen B b
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| }}</ref>
| |
| | Second-generation spectrograph
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| |-
| |
| | [[Neptune]]
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| | [[Ice giant]]
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| | 30.10
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| | 164.79 years
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| | 0.281
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| | Third-generation spectrograph
| |
| |-
| |
| | [[Earth]]
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| | [[Habitable planet]]
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| | 1.00
| |
| | 365.26 days
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| | 0.089
| |
| | Third-generation spectrograph (likely)
| |
| |-
| |
| | [[Pluto]]
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| | [[Dwarf planet]]
| |
| | 39.26
| |
| | 246.04 years
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| | 0.00003
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| | Not detectable
| |
| |}
| |
| </div>
| |
| {{-}}
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| | |
| ===For MK-type stars with planets in the habitable zone===
| |
| <div style="float:left">
| |
| {| class="wikitable"
| |
| |+<ref>{{cite web |url=http://202.127.29.4/bdep_meeting/download/talks/20July/SOsterman.pptt |title= An NIR laser frequency comb for high precision Doppler planet surveys |date=2010-10-16 |publisher=[[Chinese Academy of Sciences]] |accessdate=2010-10-16}}</ref>
| |
| !Stellar mass<br>({{Solar mass|link=yes}})
| |
| !Planetary mass<br>({{Earth mass|link=yes}})
| |
| !Lum.<br>(L<sub>0</sub>)
| |
| !Type
| |
| ![[Habitability of red dwarf systems|RHAB]]<br>([[Astronomical unit|AU]])
| |
| ![[Radial velocity|RV]]<br>(cm/s)
| |
| ![[Orbital period|Period]]<br>(days)
| |
| |-
| |
| | 0.10
| |
| | 1.0
| |
| | 8{{e|-4}}
| |
| | M8
| |
| | 0.028
| |
| | 168
| |
| | 6
| |
| |-
| |
| | 0.21
| |
| | 1.0
| |
| | 7.9{{e|-3}}
| |
| | M5
| |
| | 0.089
| |
| | 65
| |
| | 21
| |
| |-
| |
| | 0.47
| |
| | 1.0
| |
| | 6.3{{e|-2}}
| |
| | M0
| |
| | 0.25
| |
| | 26
| |
| | 67
| |
| |-
| |
| | 0.65
| |
| | 1.0
| |
| | 1.6{{e|-1}}
| |
| | K5
| |
| | 0.40
| |
| | 18
| |
| | 115
| |
| |-
| |
| | 0.78
| |
| | 2.0
| |
| | 4.0{{e|-1}}
| |
| | K0
| |
| | 0.63
| |
| | 25
| |
| | 209
| |
| |}
| |
| </div>
| |
| {{-}}
| |
| | |
| == Problems ==
| |
| | |
| [[Image:dopspec-inline.gif|thumb|500px|A representation of a star orbited by a planet. All the movement of the star is along the viewer's line-of-sight; Doppler spectroscopy will give a true value of the planet's mass.]]
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| [[Image:doppspec-above.gif|thumb|500px|In this case none of the star's movement is along the viewer's line-of-sight and the Doppler spectroscopy method will not detect the planet at all.]]
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| | |
| The major problem with Doppler spectroscopy is that it can only measure movement along the line-of-sight, and so depends on a measurement (or estimate) of the inclination of the planet's orbit to determine the planet's mass. If the orbital plane of the planet happens to line up with the line-of-sight of the observer, then the measured variation in the star's radial velocity is the true value. However, if the orbital plane is tilted away from the line-of-sight, then the true effect of the planet on the motion of the star will be greater than the measured variation in the star's radial velocity, which is only the component along the line-of-sight. As a result, the planet's [[true mass]] will be higher than expected.
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| | |
| To correct for this effect, and so determine the true mass of an extrasolar planet, radial-velocity measurements can be combined with [[astrometry|astrometric]] observations, which track the movement of the star across the plane of the sky, perpendicular to the line-of-sight. Astrometric measurements allows researchers to check whether objects that appear to be high mass planets are more likely to be [[brown dwarf]]s.<ref name="RVM"/>
| |
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| A further problem is that the gas envelope around certain types of stars can expand and contract, and some stars are [[variable star|variable]]. This method is unsuitable for finding planets around these types of stars, as changes in the stellar emission spectrum caused by the intrinsic variability of the star can swamp the small effect caused by a planet.
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| The method is best at detecting very massive objects close to the parent star — so-called "[[hot Jupiter]]s" – which have the greatest gravitational effect on the parent star, and so cause the largest changes in its radial velocity. Observation of many separate spectral lines and many orbital periods allows the [[signal to noise ratio]] of observations to be increased, increasing the chance of observing smaller and more distant planets, but planets like the Earth remain undetectable with current instruments.
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| {{clr}}
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| == See also ==
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| *[[Methods of detecting extrasolar planets]]
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| *[[Systemic (amateur extrasolar planet search project)]]
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| == References ==
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| {{reflist|2}}
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| == External links ==
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| * [http://exoplanets.org/index.html California and Carnegie Extrasolar Planet Search]
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| {{Exoplanet}}
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| [[Category:Astronomical spectroscopy]]
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