learning(goals(for(extrasolar( planets(fs(2016( ·...
TRANSCRIPT
Learning goals for extrasolar planets FS 2016
• What is the current status of exoplanet research? How many planets do we know? What are their properties?
• How can exoplanets be detected and characterized? What are the technical limitations?
• Why is exoplanet research interesting and popular? What is the main motivation for exoplanet research?
261
262
683
278
351
636
441
138
63
88
136
308
374
255
136
0 100 200 300 400 500 600 700 800
Cosmology/Fundamental physics
LSS of the Universe
Structure/Evolution galaxies
MW dynamics and evolution
Interstellar matter
Stars
Planetary systems
Search for life
Pre-biotic chemistry
Extreme states of matter
Sun and its solar system
Time domain astronomy
Astro instrumentation
Astro software
Other
Research interests vs science vision
820
361
684
285
233
390
916
752
160
153
179
0 200 400 600 800 1000
- - - - - - - - - - - -> - - - - - - - - - - - - - - ->
!!
ESO
in th
e 20
20s /
19-
22 Ja
n 20
15
Context of Exoplanets and Planet Formation in the Milky Way Sascha P. Quanz Institute for Astronomy, ETH, Zurich, Switzerland
Image credit: Nature, LYNETTE COOK
Compare to Nearby Edge-on Galaxy
Image credit: Nature, LYNETTE COOK
Origin of heavy elements
Molecular Clouds to Star Forming Cores
Planet-forming Disks Around nearby Stars
Hashimoto et al. 2011; Quanz et al. 2011,2012; Kusakabe et al, 2012; Grady et al. 2013; Folette et al. 2013; Garufi, Quanz et al. 2013/2014
-0.5
0
0.5
1
0.5 0 -0.5 -1R.A. offset (arcsecond)
Dec
. off
set (
arcs
econ
d)
N
E
AB Aur HD100546 HD97048
MWC480
AB Aur
MWC758
0.5’’ 0.4’’
SR21
...but in the last 4 years a lot of new results came out
Distance (arcsec)
Dis
tanc
e (a
rcse
c)
−1" −0.5" 0" 0.5" 1"
−1"
−0.5"
0"
0.5"
1"
−150 −100 −50 0 50 100 150
−
−
−
0
50
100
150
N
E
AO feature
Dip
a)HD169142
HD163296
Planet-forming Disks Around nearby Stars
Muto et al. 2013; Garufi, Quanz et al. 2013; Avenhaus et al. 2014; Canovas et al. 2013; Tsukagoshi et al. 2014; Mayama et al 2012; Hashimoto et a;. 2012
AB Aur
SAO206462HD135344B
SAO206462HD135344B
HD142527 HD142527
H. Canovas et al.: Near-infrared imaging polarimetry of HD 142527
Fig. 1. Processed images of HD 142527 (top row) and HD 161743 (bottom row) in H band. From left to right: intensity image (I) in logarithmicscale, Stokes Q, U and PI images in linear scale. For comparison purposes, HD 161743 has been scaled by an arbitrary factor. Units are given incounts. The area corresponding to the saturated pixels (rsat ⇤ 0.32⇧⇧) in HD 142527 has been masked out in all images. The polarized images ofHD 142527 show a complex structure, while the comparison star only shows remnant noise. In all images north is up and east is left. This appliesto all the figures in this paper.
Fig. 2. Idisk images at H band. Left: without rotating the flux-scaledHD 161743 image. Right: rotating the HD 161743 image to match thespider’s pattern (indicated by dashed-lines) in the HD 142527 image.The innermost (r ⇤ 0.67⇧⇧) regions are masked out to remove arti-facts. The white arrows point to previously identified ghosts, which areenhanced when rotating the PSF to correct for the spiders. Bar unitsare given in counts. The bright path to the east, immediately above thedotted spider line, is an artifact of the PSF-subtraction process.
PI (top row) and Idisk (bottom row) images at H (left column)and Ks band (right column). The two PI images are plotted withthe same color scale, as is done with the Idisk images in the bot-tom row. All the bright clumps in the Idisk image at Ks band arecaused by instrumental, unpolarized artifacts. The overall diskstructure recovered from the PSF-subtracted images matchesprevious images at Ks band (Fukagawa et al. 2006; Casassuset al. 2012) and L band (Rameau et al. 2012) well. The polar-ized signal inside the gap is within 3�PI of the sky background.We estimated �PI of the background by computing the medianof the standard deviation in four sky regions (5 � 5 px each) ofthe PI image. There is a marginal detection of the spiral feature(PA ⌅ 260⇥) labeled as “2” in Fig. 2 by Casassus et al. (2012).Both the PSF-subtracted and the PI images at H and Ks bandsshow two nulls or gaps at position angles of PA: [340⇥ to 10⇥](northern null) and PA: [130⇥ to 165⇥] (southern null). Inside thecavity, the best detection limit for a point source in the intensity
Fig. 3. PI (top row) and Idisk (bottom row) images at H (left column) andKs band (right column) of HD 142527. Masked area in the PI imagescover the saturate region, while in the PSF-subtracted images cover theartifact-dominated regions. The PI are plotted with the same scale toenhance di⇥erences/similarities. The same is done with the Idisk images.The bright patch in the Idisk image at north-east direction in Ks band isan artifact due to the PSF-subtraction (as it is the bright path on the eastdirection in the Idisk image at H band, see also the caption in Fig. 2).Color bar units are given in counts.
image is �mH = 5.5 mag at 0.6⇧⇧ from the central star. In polar-ized intensity, the best 3� limit is 13.5 mags/arcsec2 at the sameposition. With these limits we do not detect the HCO+ streamersclaimed by Casassus et al. (2013) and cannot verify the putativecompanion claimed by Biller et al. (2012).
4.1. Brightness asymmetries and color of the PI images
The eastern side of the disk is more extended than the westernside in the PI images at both H and Ks bands. The eastern side
A123, page 5 of 10
Sz91
2MJ1604-2130 PDS70
...but in the last 4 years a lot of new results came out
Moon exploration
Mars exploration
Io
Moons
Europa
Vesta (Dawn 17.7.2011)
Moon
Asteroid Vesta
Galileo-Observations: Ida (59 x 25 x 19 km) und Dactyl (1.5 km)
Asteroid Ida and Dactyl
iron meteorite
rocky meteorite
Meteorites
comet Wild
comet West
Comets
comet 67P/Churyumov–Gerasimenko (Tschuri)
History of extra-‐solar planet detec<ons
History of extra-‐solar planet detec<ons
History of extra-‐solar planet detec<ons
History of extra-‐solar planet detec<ons
History of extra-‐solar planet detec<ons
Today more than 5400 exoplanets (candidates) are known