The Right Instrument for your Science Case

Transcription

1 The Right Instrument for your Science Case Henri Boffin ESO Karen Humby, The Messenger

2

3 An amazing suite Imagers EFOSC2 SOFI FORS2 HAWK-I VISIR NACO SPHERE visible IR visible NB, JHKs M AO JHK, Lp AO visible, JHK Spectrographs: Resolving Power versus l ESPRESSO UVES CRIRES Multiplex FORS2 MXU KMOS IFU (24 arms) MUSE IFU 1 x1 SINFONI IFU FLAMES 130 fibers Polarimeters FORS2 EFOSC2 SOFI SPHERE NACO Interferometry PIONIER GRAVITY Resolving power FLAMES HR X-shooter LR MUSE FORS2 & VIMOS KMOS & SINFONI SPHERE Wavelength (nm) HR IR LR VISIR

4 VIRCAM Attached to VISTA, a 4m telescope Wide-field infrared imager μm Pixel: 0.34 BB and NB filters FoV: 1. 5 deg 2 in 6 pawprints 16 CCDs

5 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 OMEGACAM

6 Orion in full VISTA Optical Infrared

7 FORS2

8 FORS2 It should be called A wonderful German understatement! FOcal Reducer Fast Imager and low dispersion Single and Multi-Object Spectropolarimeter FORFISMOS

9 The Workhorse instrument in Paranal!

10 FORS Iconic Images FOV: 7 x7 Pixel scale: 0.125

11 789:"] Imaging FH/!15,/I+!5.345)4!J234K65.5+J!5*!+H/!L,031!L3)1!.34)5+-1/! I36I-63+/1!M0,!3!N05)+!*0-,I/!0M!G/,0!I060-,!OP%<!*+3,Q!RH5IH!R0-61! 45S/!3!:$T!0M!?!5)!0)/!H0-,!R5+H!13,U!*UVW!I6/3,!I0)15+50)*W!3!*//5)4! I36I-63+/1!-*5)4!+H/!L,031L3)1!M56+/,*!0M!+H/!*+3)13,1!5)*+,-./)+! ()*+,-./)+!.01/ 234)5+-1/! :"!;"< 789:"!2(F <(28:!;"< Remember: FORS2 has a LADC and narrow band filters

12 IMAGING Halley V = 28.2 FORS1+ FORS2+ VIMOS 3 nights 81 images s

13 Long-slit spectroscopy nm Slits: 0.3 to 2.5 R ~ Mag limit ~ Fleming 1 PN: host of a post-ce binary Boffin+ 12, Science

14 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)

15 Sterzik+ 12

16 Transmission Spectroscopy Transiting exoplanets Tens of ppm precision Use MXU and measure transit depths as function of wavelength Sedaghati+ 17

17 The little but older brother: EFOSC2 ESO Faint Object Spectrograph and Camera 2 FOV: 4.1 x4.1 Pixel scale: 0.12"

18 The little but older brother: EFOSC2 Imaging (BB, NB) Arp 271 Hen 2-29 PN M3-4 NGC 3132

19 The little but older brother: EFOSC2 Imaging (BB, NB) Spectroscopy MXU Polarimetry Arp 271 Spectrum of a Young Star in M17

20 The little but older brother: EFOSC2 SN 2018aca Type IA

21 µm range Imaging (0.28 /pix) - BB and NB filters. Spectroscopy: low resolution (R=600) and medium resolution (R= ), with fixed width slits of 0.6, 1 and 2. SoFI: Son of ISAAC Kilonova AT2017gfo Smartt+ 2017

22 SoFI: Son of ISAAC µm range Imaging (0.28 /pix) BB and NB filters. Spectroscopy: low resolution (R=600) and medium resolution (R= ), 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

23 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 (T exp ~ 1h, RV ~ 100m/s).

24 HD C. Lovis et al.: The HARPS search for sou C. Lovis et al.: The HARPS search for southern extra-solar planets 4 5 to 7 planets in one system: (a) y (AU) ecc 1 (b) (c) time (kyr) Fig. 8. Evolution of the eccentricities -4 of the planets -3 b (red) -2and c (green) -1 during 20 kyr for three different models. In the top picture the initial eccentricity of planet b is set at zero, but mutual gravitational perturbations 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 prevent the eccentricity of planet d to reach high values. In the bottom figure we use a model where the eccentricities of both planets were previously damped by tidal dissipation (Table 6). This last solution is stable at least for 10 Myr. 0 x (AU) Fig. 11. Long-term evolution of the HD planetary system over 10 Myr starting with the orbital solution from Table 6. The panel shows a face-on view of the system. x and y are spatial coordinates in a frame centered on the star. Present orbital solutions are traced with solid lines and each dot corresponds to the position of the planet every 100 kyr. The semi-major axes (in AU) are almost constant, but the eccentricities undergo significant variations (Table 7) amp (1 Super-Earth, with 1.4 Earth masses, orbital period of 1.18 days) 5 Neptune-like planets, with masses between 13 and 25 Earth masses, orbital periods from 6 to 600 days 1 Saturn-like planet, with 65 Earth masses, orbital period of 2200 days time (Gyr) Fig. 9. Tidal evolution of the amplitude of the proper modes u1 (red), u2 (green), u3 (blue), and u4 (pink) resulting from the tidal dissipation on planet b with k2 /Q = Hara+ 16 à 6 planets secure above do probably not reach down to the Neptune-mass range yet, preventing us from having a sufficiently complete picture of them. Nevertheless, considering the well-observed cases followed at the highest precision, the RV technique shows here its ability to study the structure of planetary systems, from gas giants to telluric planets. Lovis Fig. 7. Phased RV curves for all signals in the 7-Keplerian model. In Fig. 13 of May planets log (m (type disk; d interac ing, co lengin sistent scarce planet the fo toplan global impor Fr

25 Proxima b K 1.4 m/s M sin i 1.3 M E P = 11.2 d Anglada-Escudé + 16

26 Big Brother: ESPRESSO nm R= 120,000 up to 220,000 (1 UT) or 30,000 (4UTs) RV precision < 10 cm/s (1 UT) < 1-5 m/s (4 UTs) S/N=260 in one hour on a V=12 star (1 UT) To be offered soon! S/N = 20 on a V = 20 object in one hour (4 UTs)

27 UVES Echelle Spectrograph nm (blue arm) nm (red arm) Spectral resolution ~ 40,000 up to (blue arm) (red arm) SN 1987A in 1999

28 Rapid Response Mode Observe within minutes of discovery GRB Vreeswijk+ 107 Also for kilonovae, GW

29 Detecting CO molecules 8h spectrum of a distant quasar Detect CO molecules 11 billion ly away Srianand+ 08 Measure Temperature of Universe at this epoch: 9.15 K (in excellent agreement with Big Bang)

30 A Pristine Star Caffau+ 11 Extremely metal-poor star ~13 billion year old

31 X-SHOOTER Echelle spectrograph nm R ~ (various slit widths) Mag limit ~ 21 Three arms: UVB VIS Near-IR

32 X-SHOOTER Colliding Neutron Stars ESO/E. Pian et al./s. Smartt & epessto

33 FLAMES: multi-fibre robot nm R= with GIRAFFE (up to 130 fibres) R= with UVES (up to 8 objects) FoV: 25 diam. Fibre fed: 1 or 1.2 diam IFU also possible (2 x 3 )

34 FLAMES NGC 6752 Second generation of stars fail to enter AGB phase Campbell+ 13

35 MUSE Integral Field Spectrograph 24 spectrographs 24 x 48 = 1152 mini-slits nm R ~ 4000 Pixel scale: 0.2 FoV: 1 x 1 With or without AO (AOF)

36 MUSE: Redshift 5 Galaxy

37 Pillars of Creation (M16) McLeod+ 15 3D Structure Lifetime: 3 Myrs

38 Cluster SH : F6 8V NaI CaII CaII CaII 25 HeI HeI HeII 1: sgb[e] HeI HeI HeI HeI OI 14 25: F6 8V 26: F1 3V 2: B2 4V 12 27: F1 3V Relative Flux + Const : B3 5V 4: B8 9V 5: B6 8V 6: B7 8V 7: B8 9V 8: B7 8V 9: B8 9V 10: B8 9V 11: A1 3V 12: B8 9V 13: B8 9V 14: A3 4V 15: B9 A0V 16: B9 A1V 17: A0 4V Relative Flux + Const : F6 8V 29: F1 3V 30: F1 3V 31: F2 5V 32: F2 3V 33: F7 8V 34: G5V 35: G5V 5 18: A0 4V 19: A7 9V 20: A1 2V 2 36: G5V 37: G5V 21: A1 2V 22: A1 3V 0 23: A9V F0V Wavelength (Å) 38: G5V 0 39: G5V Wavelength (Å) Fig. 4. Spectra of the brightest cluster stars extracted from the MUSE data cube. The spectrum #1 is of MWC 137. Spectra #2 to #23 are B- and A-type stars in the cluster. Their spectral classification, indicated next to each spectrum, was based primarily on the H, H, and O I 7774 equivalent widths. Spectra #24 to #39 are F- and G-type stars. Their classification is based primarily on the Ca II 8542 and Na I 5889 equivalent widths. The numbering is consistent with Table 2 and Figure 1. Grey areas block regions of the spectra with strong residuals from the telluric bands correction. tion. We determine a systemic cluster velocity of 50±20 km s 1 For the hot stars (spectral types B and A), we based our classification mostly on H and H equivalent widths. The strength based on the radial velocities of the Paschen lines (hot stars) and Ca II and Ca I lines (cool stars). The spectra have only of O I 7774 was used to confirm the spectral subclass. The cluster does not contain any O-type stars. Two objects show weak few spectral lines and there are residuals from the nebula emission for the broad hydrogen lines. This results in less accurate radial velocity measurements than expected for the B. For the cooler stars (spectral types F and later), we based our HeI absorption and we determined their spectral type to early spectral resolution For of MUSE. each star classification in the on equivalent cluster, widths of CaII 8542 and NaI We determined the stellar spectral types with the help of the The second to last column in table Table 2 lists our spectral classifications. ESO UVES Paranal Observatory Project (POP) library of highresolution spectra (R 80000, Bagnulo et al. 2003) and the In addition to MWC 137, we found two stars with potential we have a spectrum à spectral classification à extinction à magnitude à Indo-US Library of low-resolution spectra (R 5000, Valdes et al. 2004). The spectral resolving power of a range of template spectra, covering late-o to mid-g spectral subclasses, was decreased to R to match our spectra. Equivalent widths of lines used for the spectral classification (see below) were measured in these template spectra and complemented by line equivalent widths listed in Jaschek & Jaschek (1987) and Didelon (1982). MUSE does not cover the critical wavelength regions H emission (stars #4 and #16 in Table 2). H and O I 8446 emission remain after the nebular subtraction, while other nebular lines are reasonable well removed. This may indicate circumstellar material. The hydrogen Paschen lines are very broad in absorption and suggest a high value of log g, indicating a luminosity class V and main sequence evolutionary phase. These two stars may be Be stars. However, the nebula emission varies strongly on small spatial scales and bad nebular subtraction may bluewards of 4750 Å commonly used for stellar classification of leave remnants that resemble narrow H emission. Follow-up hot stars (Walborn & Fitzpatrick 1990). The spectral range and observations with higher spectral resolution are needed to determine whether these stars are indeed Be stars. resolving power do also not permit the classification of G-type star subclasses. Our spectral classification thus only accurate The right panel of Figure 1 indicates the location of the clusterage stars on sky. It demonstrates of cluster that the higher mass stars are to within a few isochrones spectral subclasses (Table 2). A review withàspec- tra at bluer wavelengths is needed. located preferentially towards the cluster center, while the lower 4 Mehner+ 15

39 Cluster SH : F6 8V NaI CaII CaII CaII 25 HeI HeI HeII 1: sgb[e] HeI HeI HeI HeI OI 14 25: F6 8V 26: F1 3V 2: B2 4V 12 27: F1 3V Relative Flux + Const : B3 5V 4: B8 9V 5: B6 8V 6: B7 8V 7: B8 9V 8: B7 8V 9: B8 9V 10: B8 9V 11: A1 3V 12: B8 9V 13: B8 9V 14: A3 4V 15: B9 A0V 16: B9 A1V 17: A0 4V Relative Flux + Const : F6 8V 29: F1 3V 30: F1 3V 31: F2 5V 32: F2 3V 33: F7 8V 34: G5V 35: G5V 5 18: A0 4V 19: A7 9V 20: A1 2V 2 36: G5V 37: G5V 21: A1 2V 22: A1 3V 0 23: A9V F0V Wavelength (Å) 38: G5V 0 39: G5V A. Mehner et al.: A jet emerging from the Wavelength (Å) Mehner+ 15 D = 5.2 kpc 3 Myr old Fig. 4. Spectra of the brightest cluster stars extracted from the MUSE data cube. The spectrum #1 is of MWC 137. Spectra #2 to #23 are B- and 10 A-type stars in the cluster. Their spectral classification, indicated next to each spectrum, was based primarily on the H, H, and O I 7774 equivalent widths. Spectra #24 to #39 are F- and G-type stars. Their classification is based primarily on the Ca II 8542 and Na I 5889 equivalent widths. The numbering is consistent with Table 2 and Figure 1. Grey areas block regions of the spectra with strong residuals from the telluric bands correction. tion. We determine a systemic cluster velocity of 50±20 km s 1 For the hot stars (spectral types B and A), we based our classification mostly on H and 10 H equivalent Myr widths. The strength based on the radial velocities of the Paschen lines (hot stars) and Ca 6II and Ca I lines (cool stars). The spectra MWC137 have only of O I 7774 was used to confirm the spectral 15 Msubclass. The cluster does not contain any O-type stars. Two objects sun show weak few spectral lines and there are residuals from the nebula emission for the broad hydrogen lines. This results in less accurate radial velocity measurements than expected for the B. For the cooler stars (spectral types F and later), we based our HeI absorption and we determined their 15 spectral Myr type to early spectral 4resolution of MUSE. classification on the equivalent widths 10 Mof We determined the stellar spectral types with the help of the sun CaII 8542 and NaI ESO UVES Paranal Observatory Project (POP) library of highresolution spectra (R 80000, Bagnulo et al. 2003) and the Indo-US Library of low-resolution spectra (R 5000, Valdes et al. 2004). The spectral resolving power of a range of template spectra, covering late-o to mid-g spectral subclasses, was decreased0to R to match our spectra. Equivalent widths of lines used for the spectral classification (see below) were measured in these template spectra and complemented by line equivalent widths listed in Jaschek & Jaschek (1987) and Didelon M V (1982). MUSE does not cover the critical wavelength regions bluewards of 4750 Å commonly used for stellar classification of hot stars (Walborn & Fitzpatrick 1990). The spectral range and resolving power do also not permit the classification of G-type The second to last column in table Table 2 lists our spectral classifications. In addition to MWC 137, we found two stars with potential H emission (stars #4 and #16 in Table 2). H and O I 8446 emission remain after the nebular subtraction, while other nebular lines are reasonable well removed. This may indicate circumstellar material. The hydrogen Paschen lines are very broad in absorption and suggest a high value of log g, indicating a luminosity class V and main sequence evolutionary phase. These two stars may be Be stars. However, the nebula emission varies strongly on small spatial scales and bad nebular subtraction may leave remnants that resemble narrow H emission. Follow-up observations with higher spectral resolution are needed to determine whether these stars are indeed Be stars. star subclasses. Our spectral classification is thus only accurate The right panel of Figure 1 indicates the location of the cluster to within a few spectral subclasses (Table 2). A review with spectra stars on sky. It demonstrates that the higher mass stars are at bluer wavelengths is needed. located preferentially towards the cluster center, while the lower Myr 20 M sun (pre main sequence) 10 Myr 1 Myr V I Fig. 6. M V versus V I color-magnitude diagram of the brightest SH cluster stars derived from the MUSE data. Black squares are B- and J H Fig. 7 UKID

40 KMOS The octopus of Paranal But with 24 cryogenic arms and each is an IFU

41 KMOS 0.8µm to 2.5µm IZ, YJ, H, K, H+K R = IFUs in 7.2 arcmin diameter circle Each IFU: 2.8" x " x 0.2 pixels to understand how galaxies grew and evolved in the early cosmos

42 KMOS 3D MPE 3D HST and CANDELS

43 HAWK-I: High Acuity Wide field K- band Imager near-infrared µm wide-field imager Pixel scale '' 7.5 x 7.5

44 HAWK-I: High Acuity Wide field K- band Imager near-infrared µm wide-field imager Pixel scale '' 7.5 x hour integration

45 HAWK-I: High Acuity Wide field K- band Imager Y, J, H, K and 6 NB filters available

46 ESO/P. Grosbøl A gallery of Spiral Galaxies

47 AO Facility on UT4 (AOF)

48 Tarentula without/with AOF Down to 0.2 resolution à Better resolved à Deeper

49 VISIR: VLT Imager and Spectrometer Mid-Infrared imager, spectrograph N-band 8 13μm Q-band μm Pixel scale: mas FoV: 36x38 or 60x60 Spectroscopy: 350 to 25,000 for mid-infrared

50 Hot South Pole of Neptune Troposphere Stratosphere T T+6.3h

51 The Fried Egg Nebula Yellow hypergiant Huge dusty double shell ESO/E. Lagadec

52 NAOS-CONICA (NACO) μm Adaptive-optics-assisted imaging imaging polarimetry, and coronagraphy Pixel scale: 13, 27 or 54 mas Equipped with one infrared ( µm) and one visual wavefront sensor ( µm). Reference star can be off-axis! Can provide Strehl of 50% with V=12 reference star Magnitude limit ~ in J, H, K

53 Image of an Exoplanet Chauvin et al., 2005 Brown Dwarf 2M Jupiter-masses 8 million years old Giant Planet Candidate Companion (GPCC) 100 x fainter 1000 ºC 55 AU distance 5 Jupiter-masses TW Hydrae Association 230 light-years Water molecules

54 Galactic Centre

55 SINFONI Near-infrared integral field spectrograph with adaptive optics capabilities μm R ~ Pixel scale: 25 to 250 mas FoV: 0.8 x0.8 to 8 x8 Can use a Laser Guide Star Mag limit ~ 18-20

56 Galactic Centre SINFONI

57 SPHERE High-contrast Imaging (coronagraph), low-resolution spectroscopy (R~30-350), polarimetry Extreme AO: Strehl ratio of ~75% in H-band On-axis reference star (R < 13 mag) In visible and in near-ir: µm FoV: 1.73"x1.73 (IFU), 3.5 x3.5 (optical) to 11 x 11 (IR)

58 Four planets around HR 8799

59 Protoplanetary discs

60 Better than Hubble Sphere/IRDIS%

61 VY CMa, a red hyper-giant

62 PIONIER at the VLTI 4 telescopes Visibilities on 6 baselines and 4 closure phases simultaneously Highly efficient (1 point ~ 5-7 min) A typical calibrated sequence is 45 min

63 PIONIER: Measuring Stars Studied 6 symbiotic or related stars Visibilities Boffin+ 2014

64 .16, are ome rom imthe rvasets urenks ons. the into unto a tive Halbwachs+ 15 Application HIP HIP to Binaries HIP X (mas) P (days) N ± ± ± HIP HIP E HIP T 0 (JD ) N ± ± ± N -6 Y (mas) Y (mas) Y (mas) e -2 E E ± ± ± V 0 (km s ) N ± ± ± E ω 1 ( o ) Y (mas) ± ± Y (mas) ± Y (mas) Ω 1 ( o T - 2,400,000 (JD) T - 2,400,000 (JD) T - 2,400,000 (JD) ;eq.2000) ± ± ± i ( o 0 50 ) ± ± ± (O-C) X (mas) a (mas) (O-C) b (mas) RV (km/s) E N 0-5 a a (mas) Phase Phase Phase ± ± ± M 1 (M ) ± ± ± ancient measurements of the primary component. M 2 (M ) ϖ (mas) the estimator of the goodness-of-fit ± defined in Stuart & Ord ± ± (1994): Achieve ± 1% or better precision ± on stellar ± 0.075mass! n VLTI Figure 1. The combined orbits of the three SB2 observed with PIONIER. Upper row: the visual orbits; the node line is in dashes. Second row: the residuals along the semi-major axis of the error ellipsoid. Third row: the residuals along the semi-minoraxisoftheerror ellipsoid. Last row: the spectroscopic orbits; the circles refer to the primary component, and the triangle to the secondary; the large filled symbols refer to the RV measurements obtained at OHP with the Sophie spectrograph. The RV are all shifted to the zero point of the ( ) [ 1/2 ( ) 9ν χ 2 1/3 ] Figure 1. The F 2 = combined orbits of the three + 2 SB2 observed with PIONIER. Upper row: the visual orbits; the node line is in dashes. Second row: the residuals 2 along the ν semi-major 9ν 1 (1) axis of the error ellipsoid. Third row: the residuals along the semi-minoraxisoftheerror ellipsoid. Last row: the spectroscopic orbits; the circles refer to the primary component, and the triangle to the secondary; the large filled 2 0 used simulations to verify that this property is true even when the number of degree of freedom is as small as five. E N

65 GRAVITY Four-beam combiner µm (K-band) 3-mas resolution Spectroscopy R ~ 22, 500, and 4500 Main science: Study of stars in Galactic Centre

66 The wind of Eta Carinae He I Br Y complex morphology of the wind Gravity Collaboration 17

67 La Silla Paranal instruments UVES SPHERE SOFI FORS KMOS MUSE GRAVITY VISIR EFOSC2 SINFONI FLAMES PIONIER NACO HAWKI VIRCAM + OMEGACAM HARPS ESPRESSO XSHOOTER

68 Happy Observing!