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Limiting Magnitude: 17 (Texp~ 1H, RV ~ 100M/S)

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Limiting Magnitude: 17 (Texp~ 1H, RV ~ 100M/S) The Right Instrument for your Science Case Henri Boffin ESO Karen Humby, The Messenger An amazing suite Imagers EFOSC2 visible SOFI IR Spectrographs: Resolving Power versus l FORS2 visible HAWK-I NB, JHKs ESPRESSO VISIR M 100 000 NACO AO JHK, Lp UVES CRIRES SPHERE AO visible, JHK HR HR Multiplex 10 000 FLAMES X-shooter FORS2 MXU LR KMOS IFU (24 arms) VISIR Resolving power Resolving IR MUSE IFU 1’x1’ MUSE KMOS & SINFONI SINFONI IFU 1000 FLAMES 130 fibers FORS2 & SPHERE VIMOS LR Polarimeters FORS2 100 100 1000 10 000 EFOSC2 Wavelength (nm) SOFI Interferometry SPHERE PIONIER NACO GRAVITY VIRCAM Attached to VISTA, a 4m telescope Wide-field infrared imager 0.9–2.5 μm Pixel: 0.34” BB and NB filters FoV: 1. 5 deg2 in 6 pawprints 16 CCDs OMEGACAM Attached to the 2.6-metre VLT Survey Telescope (VST) Visible: 350 to 1000 nm BB and NB Filters 32 individual CCDs Pixel size: 0.21” FoV: 1 x 1 degree Orion in full VISTA Optical Infrared FORS2 FORS2 A wonderful German understatement! It should be called FOcal Reducer Fast Imager and low dispersion Single and Multi-Object Spectropolarimeter FORFISMOS The Workhorse instrument in Paranal! FORS Iconic Images FOV: 7’x7’ Pixel scale: 0.125” (2[\!<(28:!0,!Imaging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emember: FORS2 has a LADC and narrow band filters !"#$%&$'" ! IMAGING Halley V = 28.2 FORS1+ FORS2+ VIMOS 3 nights 81 images 32284 s Long-slit spectroscopy 330 – 1100 nm Slits: 0.3” to 2.5” R ~ 150 – 2600 Mag limit ~ 23 – 24 Fleming 1 PN: host of a post-CE binary Boffin+ 12, Science MXU Up to ~100 slits Slit width: 0.1” à30” Slit length < 30” slit shapes: rectangular, circular, and curved Wavelength range depends on position on CCD (x-axis) Sterzik+ 12 Transmission Spectroscopy Transiting exoplanets Tens of ppm precision Use MXU and measure transit depths as function of wavelength Sedaghati+ 17 The little but older brother: EFOSC2 ESO Faint Object Spectrograph and Camera 2 FOV: 4.1’x4.1’ Pixel scale: 0.12" The little but older brother: EFOSC2 Arp 271 Imaging (BB, NB) Hen 2-29 PN M3-4 NGC 3132 The little but older brother: EFOSC2 Arp 271 Imaging (BB, NB) Spectroscopy MXU Polarimetry Spectrum of a Young Star in M17 The little but older brother: EFOSC2 SN 2018aca Type IA SoFI: Son of ISAAC 0.9-2.5 µm range Imaging (0.28”/pix) - BB and NB filters. Spectroscopy: low resolution (R=600) and medium resolution (R=1200-1500), with fixed width slits of 0.6“, 1“ and 2”. Kilonova AT2017gfo Smartt+ 2017 SoFI: Son of ISAAC 0.9-2.5 µm range Imaging (0.28”/pix) BB and NB filters. Spectroscopy: low resolution (R=600) and medium resolution (R=1200-1500), with fixed width slits of 0.6“, 1“ and 2”. Imaging polarimetry High time-resolution imaging in burst and fast photometry mode with integration times of the order of a few tens of milliseconds via hardware windowing of the detector array. Ivanov+ 11 HARPS: The exoplanet hunter! HARPS is an exceptionally STABLE spectrograph 380 to 690 nm Resolving power: 115,000 • RV accuracy: ~ 0.5 m/s on the short term (instrument, guiding, ThAr, atmosphere); ~ 1 m/s on the medium term (2 years); • Limiting magnitude: 17 (Texp~ 1h, RV ~ 100m/s). HD 10380 C. Lovis et al.: The HARPS search for southern extra-solar planets 13 12 C. Lovis et al.: The HARPS search for southern extra-solar planets 4 0.6 5 to 7 planets in one 0.5 (a) 3 0.4 0.3 system: 0.2 2 0.1 0 0.3 1 0.25 (b) • (1 Super-Earth, with 1.4 0.2 0.15 ecc 0 0.1 Earth masses, orbital 0.05 y (AU) 0 0.3 -1 period of 1.18 days) 0.25 (c) 0.2 0.15 -2 • 5 Neptune-like planets, 0.1 0.05 0 -3 with masses between 0 2 4 6 8 10 12 14 16 18 20 time (kyr) -4 13 and 25 Earth Fig. 8. Evolution of the eccentricities-4 of the planets-3 b (red)-2 and c (green)-1 0 1 2 3 4 during 20 kyr for three different models. In the top picture the initial eccentricity of planet b is set at zero, but mutual gravitational perturba- x (AU) masses, orbital periods tions increase its value to 0.4 in less than 2 kyr (Table 3). In the middle figure we included general relativity, which calms down the eccentricity variations of the innermost planet, but still did not preventtheeccentric- ity of planet d toFig. reach high 11. values.Long-term In the bottom figure evolution we use a model of the HD 10180 planetary system over from 6 to 600 days where the eccentricities of both planets were previously damped by tidal dissipation (Table10 6). ThisMyr last starting solution is stable with at least thefor orbital 10 Myr. solution from Table 6. The panel shows Fig. 13. The 15 planetary systems with at least three known planets as • 1 Saturn-like planet, aface-onviewofthesystem.x and y are spatial coordinates in a frame of May 2010. The numbers give the minimal distance between adjacent 1 centered on the star. Present orbital solutions are traced with solid lines planets expressed in mutual Hill radii. Planet sizes are proportional to with 65 Earth masses, 0.8 and each dot corresponds to the position of the planet every 100 kyr. log (m sin i). 0.6 The semi-major axes (in AU) are almost constant, but the eccentricities undergo significant variations (Table 7). amp orbital period of 2200 0.4 (type II) through angular momentum exchange with the gaseous 0.2 disk; disk evolution and dissipation within a few Myr; dynamical days 0 0 0.2 0.4 0.6 0.8 1 interactions between protoplanets leading to eccentricitypump- time (Gyr) ing, collisions or ejections from the system. It is extremelychal- Fig. 9. Tidal evolution of the amplitude of the proper modes u1 (red), u2 lenging to build models that include all these effects in a con- (green), u3 (blue), and u4 (pink) resulting from the tidal dissipation on planet b with k2/Q = 0.0015. sistent manner, given the complicated physics involved and the Hara+ 16 à 6 planets secure scarce observational constraints available on the early stages of above do probably not reach down to the Neptune-mass range planet formation. In particular, attempts to simultaneously track yet, preventing us from having a sufficiently complete picture the formation, migration and mutual interactions of several pro- Lovis+ 2011 of them. Nevertheless, considering the well-observed casesfol- lowed at the highest precision, the RV technique shows here its toplanets are still in their infancy. Observational resultsonthe ability to study the structure of planetary systems, from gasgi- ants to telluric planets. global architecture of planetary systems may therefore provide important clues to determine the relative impact of each process. Fig. 7. Phased RV curves for all signals in the 7-Keplerian model. In From the observational point of view, the least that can be each case, the contribution of the other 6 signals has been subtracted. said is that planetary systems display a huge diversity in their properties, which after all is not surprising given their complex formation processes. Fig. 13 shows planet semi-major axes ona logarithmic scale for the 15 systems known to harbour at least three planets. Systems are shown in increasing order of their mean planetary mass, while individual planet masses are illus- Fig. 12. Possible location of an additional eighth planet in the HD 10180 trated by varying dot size. The full range of distances covered system. The stability of a small-mass particle in the system is analyzed, by each planet between periastron and apastron is denoted by 1 for various semi-major axes and eccentricities, and for K = 0.78 m s− . ablackline.Theminimaldistancebetweeneachneighbouring The stable zones where additional planets could be found are the “dark pair of planets is also given, expressed in units of the mutualHill blue” regions. radius which is defined as: 1/3 a1 + a2 m1 + m2 R , = . (10) H M 2 ! 3 M " The dynamical architecture of planetary systems is likely to ∗ convey extremely useful information on their origins. The dom- As shown by Chamberset al. (1996),the instability timescale inant planet formation scenario presently includes severalphys- of a coplanar, low-eccentricity multi-planet system is related to ical processes that occur on similar timescales in protoplane- the distance between planets, expressed in mutual Hill radii, in tary disks: formation of cores, preferentially beyond the ice line, arelativelysimplemanner,andapproximate’lifeexpectancies’ through accretion of rocky and icy material; runaway gas accre- of planetary systems can be estimated based on these separa- tion on cores having reached a critical mass, rapidly forminggi- tions, the number of planets, and their masses.
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