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Radial Velocity Detection of Planets:
II. Results
•  To date 1783 exoplanets have been discovered
•  ca 558 planets discovered with the RV method. The
others are from transit searches
•  98 are in Multiple Systems (RV)
→ exoplanet.eu
Telescope
1-m MJUO
1.2-m Euler Telescope
1.8-m BOAO
1.88-m Okayama Obs,
1.88-m OHP
2-m TLS
2.2m ESO/MPI La Silla
2.7m McDonald Obs.
3-m Lick Observatory
3.8-m TNG
3.9-m AAT
3.6-m ESO La Silla
8.2-m Subaru Telescope
8.2-m VLT
9-m Hobby-Eberly
10-m Keck
Instrument
Hercules
CORALIE
BOES
HIDES
SOPHIE
Coude Echelle
FEROS
Tull Spectrograph
Hamilton Echelle
SARG
UCLES
HARPS
HDS
UVES
HRS
HiRes
Wavelength Reference
Th-Ar
Th-Ar
Iodine Cell
Iodine Cell
Th-Ar
Iodine Cell
Th-Ar
Iodine Cell
Iodine Cell
Iodine Cell
Iodine Cell
Th-Ar
Iodine Cell
Iodine Cell
Iodine Cell
Iodine Cell
Campbell & Walker: The Pioneers of RV Planet Searches
1988:
1980-1992 searched for planets around 26
solar-type stars. Even though they found
evidence for planets, they were not 100%
convinced. If they had looked at 100 stars
they certainly would have found
convincing evidence for exoplanets.
Campbell, Walker, & Yang 1988
„Probable third body variation of 25 m s–1, 2.7 year
period, superposed on a large velocity gradient“
ε Eri was a „probable variable“
The first extrasolar planet around a normal star: HD 114762 with
Msini = 11 MJ P = 84 d discovered by Latham et al. (1989)
Filled circles are data taken at McDonald Observatory using the
telluric lines at 6300 Ang as a wavelength reference
51 Pegasi b: The Discovery that Shook up the
Field
Period = 4,3 Days
Semi-major axis = 0,05 AU (10
Stellar Radii!)
Mass ~ 0,45 MJupiter
Discovered by Michel Mayor & Didier
Queloz, 1995
Rate of Radial Velocity Planet Discoveries
51 Peg
Global Properties of Exoplanets:
Mass Distribution
The Brown Dwarf Desert
Planet: M < 13 MJup → no nuclear burning
Brown Dwarf: 13 MJup < M < ~80 MJup → deuterium burning
Star: M > ~80 MJup → Hydrogen burning
Brown Dwarf Desert: Although there are ~100-200
Brown dwarfs as isolated objects, and several in
long period orbits, there is a paucity of brown
dwarfs (M= 13–50 MJup) in short (P < few years) as
companion to stars
An Oasis in the Brown Dwarf Desert: HD 137510 = HR 5740
Brown Dwarfs versus Planets
Bump due to
deuterium
burning
The distinction between brown dwarfs and planets is
vague. Until now the boundary was taken as ~ 13 MJup
where deuterium burning is possible. But this is
arbitrary as deuterium burning has little influence on the
evolution of the brown dwarf compared to the planet
A better boundary is to use the different distributions
between stars and planets:
By this definition the boundary between
planets and non-planets is 20 MJup
Mass Distribution at Low Masses
A note on the naming convention:
Name of the star: 16 Cyg
If it is a binary star add capital letter B, C, D
If it is a planet add small letter: b, c, d
55 CnC b : first planet to 55 CnC
55 CnC c: second planet to 55 CnC
16 Cyg B: fainter component to 16 Cyg binary system
16 Cyg Bb: Planet to 16 Cyg B
The IAU has yet to agree on a rule for the naming of
extrasolar planets
Semi-Major Axis Distribution
The lack of long period planets is a selection effect since these take a
long time to detect
The short period planets are also a selection effect: they are the
easiest to find and now transiting surveys are geared to finding these.
Eccentricity versus Orbital Distance
Note that there are few highly eccentric orbits close into the star. This
is due to tidal forces which circularizes the orbits quickly.
Eccentricity distribution
Fall off at high eccentricity may be partially due to an observing
bias…
e=0.4
e=0.6
e=0.8
ω=0
ω=90
ω=180
…high eccentricity orbits are hard to detect!
For very eccentric
orbits the value of the
eccentricity is is often
defined by one data
point. If you miss the
peak you can get the
wrong mass!
At opposition with Earth would
be 1/5 diameter of full moon,
12x brighter than Venus
ε Eri
16 Cyg Bb was one of the first
highly eccentric planets discovered
2 ´´
Comparison of some eccentric orbit planets to our solar system
Mass versus Orbital Distance
There is a relative lack of massive close-in planets
Classes of planets: 51 Peg Planets: Jupiter mass
planets in short period orbits
Another short period giant planet
Classes of planets: 51 Peg Planets
• 
~40% of known extrasolar planets are
51 Peg planets with orbital periods of
less than 20 d. This is a selection effect
due to:
1.  These are easier to find.
2.  RV work has concentrated on
transiting planets
• 
0.5–1% of solar type stars have giant
planets in short period orbits
• 
5–10% of solar type stars have a giant
planet (longer periods)
Classes of planets: Hot Neptunes
Santos et al. 2004
McArthur et al. 2004
Butler et al. 2004
Note that the scale on the yaxes is a factor of 100
smaller than the previous
orbit showing a hot Jupiter
Msini = 14-20 MEarth
If there are „hot Jupiters“ and „hot Neptunes“ it makes sense that
there are „hot Superearths“
CoRoT-7b
Mass = 7.4 ME
P = 0.85 d
Hot Superearths were discovered by space-based transit
searches
Earth-mass Planet: Kepler 78b
Pepe et al. 2013,
Howard et al. 2013
Mass = 1.31± 0.25 MEarth (Amplitude = 1.34 m/s)
Period = 8.5 hours
Classes of Planets: The Massive Eccentrics
•  Masses between 7–20 MJupiter
• Eccentricities, e > 0.3
•  Prototype: HD 114762 discovered in 1989!
m sini = 11 MJup
Red: Planets with masses < 4 MJup
Blue: Planets with masses > 4 MJup
Planet-Planet Interactions?
Initially you have two giant
planets in circular orbits
These interact gravitationally.
One is ejected and the
remaining planet is in an
eccentric orbit
Lin & Ida, 1997, Astrophysical Journal, 477, 781L
Classes: Planets in Binary Systems
Why should we care about binary stars?
•  Most stars are found in binary systems
•  Does binary star formation prevent planet
formation?
•  Do planets in binaries have different characteristics?
•  What role does the environment play?
•  Are there circumbinary planets?
Some Planets in known Binary Systems:
For more examples see Mugrauer & Neuhäuser 2009, Astronomy &
Astrophysics, vol 494, 373 and references therein
There are very few planets in close binaries. The
exception is γ Cep.
If you look hard enough, many exoplanet host
stars in fact have stelar companions
A new stellar
companion to the
planet hosting
star HD 125612
Mugrauer & Neuhäuser 2009
Approximately 17% of the exoplanet hosting stars have stellar
companions (Mugrauer & Neuhäuser 2009). Most of these are in wide
systems.
γ Cep Ab: A planet that
challenges formation theories
The first extra-solar Planet may
have been found by Walker et al. in 1988 in a
binary system:
Ca II is a measure of stellar activity (spots)
γ Cephei
Planet
Period
Msini
2.47 Years
1.76 MJupiter
e
a
K
0.2
2.13 AU
26.2 m/s
Binary
Period
Msini
56.8 ± 5 Years
~ 0.4 ± 0.1 MSun
e
a
0.42 ± 0.04
18.5 AU
K
1.98 ± 0,08 km/s
γ Cephei
Primary star (A)
Secondary Star (B)
Planet (b)
The planet around γ Cep is difficult to form and on the
borderline of being impossible.
Standard planet formation theory: Giant planets form beyond
the snowline where the solid core can form. Once the core is
formed the protoplanet accretes gas. It then migrates
inwards.
In binary systems the companion truncates the disk. In the
case of γ Cep this disk is truncated just at the ice line. No ice
line, no solid core, no giant planet to migrate inward. γ Cep
can just be formed, a giant planet in a shorter period orbit
would be problems for planet formation theory.
The interesting Case of 16 Cyg B
Effective Temperature: A=5760 K, B=5760 K
Surface gravity (log g): 4.28, 4.35
Log [Fe/H]: A= 0.06 ± 0.05, B=0.02 ± 0.04
16 Cyg B has 6 times less Lithium
These stars are identical and are „solar twins“. 16 Cyg B
has a giant planet with 1.7 MJup in a 800 d period
Kozai Mechanism: One Explanation for the high
eccentricty of 16 Cyg B
Two stars are in long period orbits around each other.
A planet is in a shorter period orbit around one star.
If the orbit of the planet is inclined, the outer planet can „pump up“ the
eccentricity of the planet. Planets can go from circular to eccentric orbits.
This was first investigated by Kozai who showed that satellites in orbit
around the Earth can have their orbital eccentricity changed by the
gravitational influence of the Moon
Kozai Mechanism: changes the inclination and
eccentricity
Planetary Systems: ~ 100 Multiple Systems
The first:
Some Extrasolar Planetary Systems
Star
P (d) MJsini a (AU) e
HD 82943 221 0.9
0.7
0.54
444 1.6
1.2
0.41
GL 876
47 UMa
30
61
1095
2594
0.6
2.0
2.4
0.8
HD 37124 153
0.9
550
1.0
55 CnC
2.8
0.04
14.6 0.8
44.3 0.2
260
0.14
5300 4.3
Ups And 4.6
0.7
241.2 2.1
1266 4.6
HD 108874 395.4 1.36
1605.8 1.02
HD 128311 448.6 2.18
919 3.21
HD 217107 7.1 1.37
3150 2.1
0.1
0.2
2.1
3.7
0.27
0.10
0.06
0.00
0.5
2.5
0.04
0.1
0.2
0.78
6.0
0.06
0.8
2.5
1.05
2.68
1.1
1.76
0.07
4.3
0.20
0.40
0.17
0.0
0.34
0.2
0.16
0.01
0.28
0.27
0.07
0.25
0.25
0.17
0.13
0.55
Star
P (d) MJsini
HD 74156 51.6
1.5
2300
7.5
HD 169830 229
2.9
2102
4.0
HD 160691 9.5
0.04
637
1.7
2986
3.1
HD 12661
HD 168443
HD 38529
HD 190360
HD 202206
HD 11964
263
1444
58
1770
14.31
2207
17.1
2891
255.9
1383.4
37.8
1940
2.3
1.6
7.6
17.0
0.8
12.8
0.06
1.5
17.4
2.4
0.11
0.7
a (AU)
0.3
3.5
0.8
3.6
0.09
1.5
0.09
e
0.65
0.40
0.31
0.33
0
0.31
0.80
0.8
2.6
0.3
2.9
0.1
3.7
0.13
3.92
0.83
2.55
0.23
3.17
0.35
0.20
0.53
0.20
0.28
0.33
0.01
0.36
0.44
0.27
0.15
0.3
The 5-planet System around 55 CnC:
0.17MJ
5.77 MJ
•
0.11 MJ
Red lines: solar system plane orbits
0.82MJ
•
•0.03M
J
The Planetary System around GJ 581
16 ME
7.2 ME
5.5 ME
Inner planet 1.9 ME
Can we find 4 planets in
the RV data for GL 581?
Note: for Fourier analysis
we deal with frequencies
(1/P) and not periods
ν1 = 0.317 cycles/d
ν2 = 0.186
ν3 = 0.077
ν4 = 0.015
Yes!
The Period04 solution:
Published solution:
P1 = 5.37 d, K = 12.7 m/s
P1 = 5.37 d, K = 12.5 m/s
P2 = 12.92 d, K = 3.2 m/s
P2 = 12.93 d, K = 2.63 m/s
P3 = 66.7 d, K = 2.7 m/s
P3 = 66.8 d, K = 2.7 m/s
P4 = 3.15, K = 1.05 m/s
P4 = 3.15, K = 1.85 m/s
σ=1.2 m/s
σ=1.53 m/s
Resonant Systems Systems
Star
P (d) MJsini a (AU) e
HD 82943 221 0.9
0.7
0.54
444 1.6
1.2
0.41
→
GL 876
30
61
55 CnC
14.6
44.3
2:1
0.6
2.0
0.1
0.2
0.27
0.10
→ 2:1
0.8
0.2
0.1
0.2
0.0
0.34
→ 3:1
HD 108874 395.4 1.36
1605.8 1.02
1.05
2.68
0.07
0.25
→ 4:1
HD 128311 448.6 2.18
919 3.21
1.1
1.76
0.25
0.17
→ 2:1
2:1 → Inner planet makes two orbits for
every one of the outer planet
Eccentricities
•
Period (days)
Red points: Systems
Blue points: single planets
Mass versus
Orbital Distance
Eccentricities
Red points: Systems
Blue points: single planets
Idea: If you divide the disk mass among several
planets, they each have a smaller mass?
Exoplanets around low mass stars (Mstar < 0.4 Msun)
Programs:
•  ESO UVES program (Kürster et al.): 40 stars
•  HET Program (Endl & Cochran) : 100 stars
•  Keck Program (Marcy et al.): 200 stars
•  HARPS Program (Mayor et al.):~200 stars
Results:
•  ~15 planets around low mass (M = 0.15-0.4 Msun)
•  Giant planets (2) around GJ 876. Giant planets
around low mass M dwarfs seem rare
•  Hot neptunes around several → low mass start tend
to have low mass planets
Transiting surveys are finding more planets around M dwarfs
GL 876 System
1.9 MJ
0.6 MJ
Inner planet 0.02 MJ
Exoplanets around massive stars
Difficult with the Doppler method because more massive
stars have higher effective temperatures and thus few
spectral lines. Plus they have high rotation rates. A way
around this is to look for planets around giant stars. This
will be covered in „Planets around evolved stars“
Result: Only a few planets around early-type, more massive
stars, and these are mostly around F-type stars (~ 1.4 solar
masses)
Galland et al. 2005
HD 33564
M* = 1.25 solar masses
m sini = 9.1 MJupiter
P = 388 days
e = 0.34
F6 V star
A Planet around an F star from the Tautenburg Program
HD 8673
Mplanet = 14.6 MJup
Period = 4.47 Years
ecc = 0.72
P = 328 days
Msini = 8.5 Mjupiter
e = 0.24
Scargle Power
An F4 main sequence
star from the
Tautenburg program
M* = 1.4 M
Frequency (c/d)
ε Eri: A „complete“ System
•  Long period planet
•  Very young star
•  Has a dusty ring
•  Nearby (3.2 pcs)
•  Astrometry (1-2 mas)
•  Imaging (Δm =20-22 mag)
•  Other planets?
Clumps in Ring can be
modeled with a planet here
(Liou & Zook 2000)
Radial Velocity Measurements of ε Eri
Hatzes et al. 2000
Large scatter is because this is an active star. It has been argued
that this is not a planet at all, but rather the signal due to activity.
Scargle Periodogram of ε Eri Radial velocity measurements
False alarm probability ~ 10–8
Scargle Periodogram of Ca II measurements
Figure 10 from The HARPS-TERRA Project. I. Description of the Algorithms, Performance, and New Measurements on
a Few Remarkable Stars Observed by HARPS
Guillem Anglada-Escudé and R. Paul Butler 2012 ApJS 200 15 doi:10.1088/0067-0049/200/2/15
Hatzes et al. 2000
Anglada-Escude & Butler 2011
Period: 2501 ± days
Period: 2651 ± 36 days
Eccentricity: 0.61 ± 04
Eccentricity: 0.40 ± 0.1
ω : 49 ± 4degrees
ω : 141 ± 10 degrees
K: 19.0 ± 1.7 m/s
K: 11.8 ± 1.1 m/s
msini : 0.86 MJupiter
msini : 0.64 MJupiter
Anglada-Escude & Butler argue
that the variations are due to an
activity cycle.
False Planets
or
How can you be sure that you have actually
discovered a planet?
HD 166435
In 1996 Michel Mayor announced at a conference in
Victoria, Canada, the discovery of a new „51 Peg“
planet in a 3.97 d. One problem…
HD 166435 shows the same period in in
photometry, color, and activity indicators.
This is not a planet!
Fake Planets
What can mimic a planet in Radial Velocity Variations?
1.  Spots or stellar surface structure
2.  Stellar Oscillations
3.  Convection pattern on the surface of the star
4.  Noise
Radial Velocity (m/s)
Starspots can produce Radial Velocity Variations
Spectral Line distortions
in an active star that is
rotating rapidly
10
-10
0
0.2
0.4
0.6
Rotation Phase
0.8
Activity Effects: Convection
Hot rising cell
Cool sinking lane
• The integrated line profile is distorted.
• The ratio of dark lane to hot cell areas changes
with the solar cycle
This is a Jupiter!
RV changes can be as large as 10 m/s
with an 11 year period
One has to worry even about the nature
long period RV variations
Tools for confirming planets: Photometry
Starspots are much cooler than
the photosphere
Light Variations
Color Variations
Relatively easy to measure
Tools for confirming planets: Ca II H&K
Active star
Inactive star
Ca II H & K core emission is a measure of magnetic activity:
HD 166435
Ca II emission
measurements
Tools for confirming planets: Bisectors
Bisectors can measure the line shapes and tell you about
the nature of the RV variations:
Curvature
Span
What can change bisectors:
•  Spots
•  Pulsations
•  Convection pattern on star
Spots produce an „anti-correlation“ of Bisector
Span versus RV variations:
Correlation of bisector span with radial velocity for HD 166435
How do you know you have a planet?
1.  Is the period of the radial velocity reasonable? Is it the
expected rotation period? Can it arise from pulsations?
• 
E.g. 51 Peg had an expected rotation period of ~30
days. Stellar pulsations at 4 d for a solar type star
was never found
2.  Do you have Ca II data? Look for correlations with RV
period.
3.  Get photometry of your object
4.  Measure line bisectors
5.  And to be double sure, measure the RV in the infrared!
The Non-Planet around TW Hya
Figueira et al. 2010, Astronomy
and Astrophysics, 511, 55
A constant star
Points: IR measurements, Solid line is the
orbital solution using optical radial velocity
measurements, but with one-third the
optical amplitude → No planet!
Period = 3.24 d
K = 0.5 m/s
Msini = 1.13 MEarth
FAP = 0.02%
Is Alpha Cen Bb really there?
Claimed detection:
Dumusque et al. 2012
False alarm probability (FAP) ~ 0.02 %
False alarm probability = 0.4
False alarm probability = 0.00010
Data
Fake Planet
Maybe not!
Radial Velocity Planets
Period in years → 30 90
Red line: Current detection limits
Green line detection limit for a precision of 1 m/s
1000
Summary
Radial Velocity Method
Pros:
•  Most successful detection method
•  Gives you a dynamical mass
•  Distance independent
• 
Important for transit searches
Summary
Radial Velocity Method
Cons:
• 
Only effective for cool stars.
• 
Most effective for short (< 10 – 20 yrs)
periods
• 
Only high mass planets, but getting closer to
Earth mass planets
• 
Only get projected mass (msin i)
• 
Other phenomena (pulsations, spots, etc.) can
mask as an RV signal. Must be careful in the
interpretation
The Radial Velocity Method is successful, but highly
biased – we only know about planets around solartype stars!
Summary of Exoplanet Properties from RV
Studies
•  ~10 % of normal solar-type stars have giant planets
•  < 1% of the M dwarfs stars (low mass) have giant planets, but may have
a large population of neptune-mass planets
→ low mass stars have low mass planets, high mass stars have more
planets of higher mass → planet formation may be a steep function of
stellar mass
•  0.5–1% of solar type stars have short period giant plants
•  Exoplanets have a wide range of orbital eccentricities (most are not in
circular orbits)
•  Massive planets tend to be in eccentric orbits and have large orbital radii