AGA5802 High resolu2on spectroscopy: echelle Echelle spectrographs Applica(ons

Transcrição

1 AGA5802 High resolu2on spectroscopy: echelle Echelle spectrographs Applica(ons Bibliography: To Measure the Sky, Kitchin, Lena and others... Prof. Jorge Meléndez 1

2 Para obter alta resolução espectral (alta dispersão) com uma rede : 1. Usamos uma rede de maior resolução (>> 1000 linhas por mm) ou aumentamos f COL 2. Trabalhamos em altas ordens m à echelle σ 2

3 High resolu2on 1: redes de difração with many lines/mm + increase f COL Fenda rede Colimador Problem : small spectral coverage Roy & Clarke 3

4 High resolu2on 1: redes de difração com muitas linhas/mm Exemplo: espectrógrafo Coudé OPD (LNA) Å R (600nm) Comparação : Echelle HIRES cobertura 4000Å ou 40 X maior 4

5 High resolu2on 2: espectrógrafo [po echelle Kitchin Rede de difração echelle Blazing angle is increased para o[mizar a observação de ordens maiores (m ~ ) à maior resolução Typical gra[ng 31 lines/mm Problem : order overlapping? 5

6 Solução para mistura de ordens: cross disperser (pode ser um prisma ou uma rede) cross disperser (rede ou prisma) 6 CCD

7 Echelle spectrographs Cross disperser could be a gra[ng or a prism. Serve para separar as ordens muito altas 7

8 Exemplo : HIRES spectrograph no KECK Cross disperser could be a gra[ng or a prism. Serve para separar ordens muito altas. 8

9 Echelle orders 9

10 Echelle orders : extracted 10

11 Mike Spectrograph at 6,5m Magellan (Las Campanas) Blue Side Red Side effec2ve focal ra2o f/3.9 f/3.6 scale at CCD 8.2 pix/" (0.12"/pix) 7.5 pix/sec (0.13"/pix) Å/pixel (unbinned) ~0.02 ~0.05 detector 2048x4096 (15µm pix) 2048x4096 (15µm pix) gain ~0.47 e-/dn ~1.0 e-/dn Readnoise ~2 e-/pix ~3.5e-/pix Dark current ~5 DN/pix/hr ~2 DN/pix/hr CCD efficiency Q.E. Wavelength range* Å Å Resolu2on (0.35"slit) 83,000 65,000 Resolu2on (1.0" slit) 28,000 22,000 The tangent of the blazing angle = R#. Thus blazing angle for the R4 gra2ng is 76 O Echelle gra2ng R2.4 R2 Prism (cross-disperser) Fused Silica (2 prisms) PBM2 (1 prism) 11

12 Espectrógrafo MIKE tem 2 braços 12

13 Slits available at MIKE Aperture Pairs (separa[on 3"): x 0.35 (for focusing) x x x x x x x x x x x x x x x 2.00 Single Slits: x x x x x x

14 14

15 MIKE Blue ThAr calibra[on arc 15

16 Magellan ultra high precision study of solar twins - Magellan 6,5m Clay Telescope & MIKE spectrometer - R = S/N = 450 per pixel - coverage nm - Solar spectrum: Vesta - 3 nights of observations Observations of the solar twin 18 Sco BLUE frame RED frame 16

17 Magellan ultra high precision study of solar twins Observations of the solar twin 18 Sco BLUE frame 17

18 Magellan ultra high precision study of solar twins Observations of the solar twin 18 Sco RED frame 18

19 Example of MIKE spectra of solar twins (total spectral coverage 3350 A -1µm) Small part ( nm) of solar twin & Sun s spectra Meléndez et al

20 Planning observa2ons with echelle spectrographs 1. Spectral coverage : quais as linhas importantes a detetar? 1 braço ou 2 braços? 2. Resolving power : suficiente para resolver as linhas de interesse? Se houver mais de 1 braço, verificar se o R é adequado em ambos 3. S/N : telescópio + instrumento são adequados? 20

21 High resolu[on spectroscopy of solar twins with the Keck telescope. Observa[on, undergrad research experience, publica[on, science populariza[on, and having a good [me in Hawaii 21

22 22

23 WAIMEA KONA Mauna Kea HILO 23

24 CFHT Gemini N. U. Hawaii 2.2m UKIRT NASA IRTF Keck II Keck I Subaru 24

25 Ar[s[c image of TMT on Mauna 25 Kea

26 Keck headquarters WAIMEA KONA Mauna Kea HILO Gemini headquarters (bad side of Hawaii; chove muito) 26

27 hbp://www2.keck.hawaii.edu/ observing/summit.html It is possible to arrange a day[me visit to the summit for observers working from Waimea. The visit should be scheduled during a weekday, not on holidays or weekends. 27

28 28 htp://keckobservatory.org/gallery/full/keck_telescopes/71

29 Keck telescope 29

30 30 Jorge (right) & student Damian Fabbian (lew) at the Keck prime focus cage

31 31

32 Sunset from Waikiki January

33 33

34 HIRES no Keck I hip://www2.keck.hawaii.edu/inst/hires/ Somente 1 braço : escolher HIRESb ou HIRESr 34

35 35

36 HIRES CCD data format Mosaico de 3 CCDs, cada um de 2048 x 4096 pixels (1 pixel = 15um) RED GREEN BLUE 6144 pixels 4096 pixels 36

37 HIRES Echelle Format Simulator hip://www2.keck.hawaii.edu/inst/hires/webech/efs.html Cross disperser (XD) angle = 0,247 Echelle angle = 0,0 Ordem Å 8365 Å CCD Å 6917 Å CCD Å 5282 Å CCD Å 3897 Å 37

38 HD : a minha primeira gêmea solar 38

39 Header da imagem hires1851.fits INSTRUME= 'HIRES' UTC = '12:22:40.24' DATE-OBS= ' ' XDISPERS= 'RED ' XDANGL = DEC = '+58:29:19.4' EQUINOX = ' ' HA RA ST = '+22:37:54.36' = '11:21:28.26' = '09:59:45.87' UTC-END = '12:25:11.39' DATE-END= ' ' CCDPSIZE= '[1:2048,1:4096]' OUTDIR = '/s/sdata125/hires5/19jan2006' OUTFILE = 'hires ' FRAMENO = 1851 EXPTIME = 150 seconds OBSERVER= 'J. Melendez' OBJECT = 'hd 98618' DATE_BEG= ' T12:22:39' AIRMASS = '1.33 ' DATE_END= ' T12:25:09' MJD = ' ' DECKNAME= 'E4 ' (fenda 0,40 x 7,0 TARGNAME= 'HD 98618' define o poder resolvente) TELESCOP= 'Keck I ECHANGL = CCDGAIN = 'low ' FIL1NAME= 'kv389 ' 39

40 Resolving power vs. slit width φ s HIRES spectrograph on the 10m Keck I telescope Decker name Length (") Width (") Resolu2on R (calculated) Resolu2on R (measured*) Resolu2on R (measured+) B ,000 67,000 66,400 B ,000 67,000 66,400 B ,000 67,000 66,400 B ,000 67,000 66,400 B ,000 49,000 50,000 C ,000 49,000 50,000 C ,000 49,000 50,000 C ,000 49,000 50,000 C ,000 37,000 37,500 C ,000 37,000 37,500 D ,000 37,000 37,500 D ,000 37,000 37,500 D ,000 24,000 24,700 D ,000 24,000 24,700 D pinhole E ,000 84,000 86,600 E ,000 84,000 86,600 E ,000 84,000 86,600 E E ,000 52,000 52,000 DECKER serve para fixar o comprimento da fenda ou comprimento e largura. No ul2mo caso reemplaza a fenda * Using UV cross-disperser. Average of 5 Th/Ar lines near 4100 A. + Using Red cross-disperser. Average of 4 Th/Ar lines near 5240 A. Segundo minhas medições R ~

41 Iden2fiers (16): HD HIP

42 htp://www2.keck.hawaii.edu/inst/hires/etc.html We are adop[ng V = 7,646, but this is in the Johnson system. Be careful! What we need are AB magnitudes, i.e., U AB,B AB,V AB, R AB, etc 42

43 V = 7,646 slit = 0,4 seeing 0,6 exp[me = 150 s S/N (per pixel) V 43

44 To do it properly magnitudes should be in the AB system V(AB) = V (+/ ) B(AB) = B (+/ ) Rc(AB) = Rc (+/ ) Ic(AB) = Ic (+/ ) V(AB) = B(AB) = Rc(AB) = Ic(AB) = HD HIP

45 B R V Here we are using AB magnitudes for HD

46 Header da imagem hires1851.fits INSTRUME= 'HIRES' UTC = '12:22:40.24' DATE-OBS= ' ' XDISPERS= 'RED ' XDANGL = DEC = '+58:29:19.4' EQUINOX = ' ' HA RA ST = '+22:37:54.36' = '11:21:28.26' = '09:59:45.87' UTC-END = '12:25:11.39' DATE-END= ' ' CCDPSIZE= '[1:2048,1:4096]' OUTDIR = '/s/sdata125/hires5/19jan2006' OUTFILE = 'hires ' FRAMENO = 1851 EXPTIME = 150 seconds OBSERVER= 'J. Melendez' OBJECT = 'hd 98618' DATE_BEG= ' T12:22:39' AIRMASS = '1.33 ' DATE_END= ' T12:25:09' MJD = ' ' DECKNAME= 'E4 ' (fenda 0,40 x 7,0 TARGNAME= 'HD 98618' define o poder resolvente) TELESCOP= 'Keck I ECHANGL = CCDGAIN = 'low ' FIL1NAME= 'kv389 ' 46

47 hip://www2.keck.hawaii.edu/inst/hires/filter_choices.html É possível observar H e K (394 nm) e ao mesmo tempo o tripleto de oxigênio em 777 nm e o dubleto de Al em 784 nm? 47

48 HIRES mosaic for solar twin HD Second order (cross-disperser gra[ng) contamina[on 48

49 Contamina2on by second order 49

50 MAKEE hires pipeline (redução automá[ca) CCD 1 (faltam algumas ordens) Wavelength (A) 50

51 MAKEE hires pipeline (redução automá[ca) CCD 2 Wavelength (A) 51

52 MAKEE hires pipeline (redução automá[ca) CCD 3 Esta ordem tem muito pouca contaminação Úl[mas 3 ordens ligeiramente contaminadas! Wavelength (A) 52

53 Header da imagem hires1851.fits INSTRUME= 'HIRES' UTC = '12:22:40.24' DATE-OBS= ' ' XDISPERS= 'RED XDANGL = DEC = '+58:29:19.4' EQUINOX = ' ' HA RA ST = '+22:37:54.36' = '11:21:28.26' = '09:59:45.87' AIRMASS = '1.33 ' MJD = ' ' ' UTC-END = '12:25:11.39' DATE-END= ' ' CCDPSIZE= '[1:2048,1:4096]' OUTDIR = '/s/sdata125/hires5/19jan2006' OUTFILE = 'hires ' FRAMENO = 1851 EXPTIME = 150 seconds OBSERVER= 'J. Melendez' OBJECT = 'hd 98618' DATE_BEG= ' T12:22:39' DATE_END= ' T12:25:09' DECKNAME= 'E4 ' (fenda 0,40 x 7,0 define o poder resolvente) ECHANGL = TARGNAME= 'HD 98618' FIL1NAME= 'kv389 ' 53 TELESCOP= 'Keck I

54 Stromlo Summer Scholar (Iniciação C.) Ka[e Dodds Eden 54

55 Observações feitas em 2006 January 20!!! 55

56 Iniciação (Summer Scholar): gêmeas solares Mestrado de 1 ano (Honours): teoria MOND (alterna[va a matéria escura) 56 Doutorado na Alemanha (observacional, centro Galác[co)

57 HD 98618: Destaque na imprensa

58 Radial velocity and planets 58

59 Planeta em torno de HD

60 Dois planetas around Ups And 60