amateur astronomical spectroscopy amateur astronomical... · solar spectrum william wollaston...
TRANSCRIPT
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AmateurAmateurAstronomicalAstronomicalSpectroscopySpectroscopy
Olivier [email protected]
---April 15th, 2011
-- NEAIC ; NY, USA --
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the “menu”...
• Starting in spectroscopy(with some history)
• Equipment
• Educational
• Pro/Am projects
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15/04/11 (c) 2006 - Shelyak Instruments 3Starting in spectroscopy
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Light & colors
➢Isaac Newton (1642-1726)➢a pionnieer➢1670: prisme's experience➢Circular “slit” of 6mm: λ/∆λ ~10 !
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Light is a wave
➢Thomas Young (1773-1829)➢Wave interpretation of light (1801)➢Worked with grating with 20 grooves/mm
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Electromagnetic spectrum
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Solar spectrum
➢William Wollaston (1766-1828)➢~150 years after Newton !➢First observation (in 1802) of dark lines➢Demonstrated the importance of the slit width
➢Joseph Fraunhofer (1787-1826)➢Manufacturer of high quality glasses➢A, B (Hα), C, D (sodium doublet)... H, K (Calcium) lines➢Catalog of ~600 raies in 1814➢Also observed planets and some stars !
➢Edmon Becquerel (1820-1891)➢First photography of the solar spectrum (June 13th, 1842)
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15/04/11 (c) 2006 - Shelyak Instruments 8
Sodium in all shape !
Sirius
Sun
Street lamp
Match
Salt
Pickel !
(c) C. Buil / Benoit Minster
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Chemical analysis & spectroscopy➢Léon Foucault (1819-1868)
➢Comparison between spectra on Earth and solar spectrum (sodium lines, 1849)
➢Gustav Kirchhoff➢In parallel, he made the experiment with salt and published in 1859 that sodium should exist on solar atmosphere!➢A key theoritical result: Kirchhoff laws
➢Robert Bunsen (1811-1899)➢Heidelberg university like Kirchhoff➢Together, they published in 1860 a paper on « chemical analysis by spectroscopic observation », then in 1861-1863 the analysis of several chemical elements and their work on the solar spectrum
➢...Spectroscopy was born...
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Kirchhoff's laws
A continuous spectra is emitted by any solid of gazeous body under high presure and high temperature. Stars are, under first approximation, like black body whose continuous spectra has a shape which depends on its surface temperature;
Absorption line spectra: a low pressure low temperature gaz crossed by a continuous light absorbs some photons. Spectra then shows dark lines in front of the continuous spectra;
Emission line spectra: a low pressure high temperature gaz emits a light made of few radiations, characteristics of the atoms that constitutes this gaz. Each chemical element has its own line spectra, true identity card of its composition and state.
1
2
3
1
2
3
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Informations from Planck profile
➢Stefan's law:Intensity (below the curve) = Constant * T4
➢Wien's law:λ max * Temperature = Constant
(2900 µm.K)
==>Temperature = Color !!!
Visible domain= 400-700nm (4000A-7000A)
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Black body profile
1000 2000 3000 4000 5000 6000 7000 8000 9000 10000
Profil de Plank
Longueur d'onde (angstroms)
Inte
nsité
12.000 K10.000 K
8.000 K5.000 K
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The simpliest spectroscope
Converging beam from telescope
Zero order
First order->spectrum !
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Multiple way to setup
As a filter(ex: front of webcam)
Front of objectiveAs a filter(ex: front of digital SLR)
(R.Leadbeater)
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30sec digital SLR shot
Sirius Spectrum – Buthier workshop 2007
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Measure temperature
Altair (A7V): 10500K
Albireo B (B8Ve): 22000KRegulus (B7V): 30000K
Antares (M1.5Iab-b): 3000K
Albireo A (K3II+...): 5000K
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Visible: a small window
Source: Getting the measure of the stars (WA Cooper & EN Walker)
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Kirchhoff's laws
A continuous spectra is emitted by any solid of gazeous body under high presure and high temperature. Stars are, under first approximation, like black body whose continuous spectra has a shape which depends on its surface temperature;
Absorption line spectra: a low pressure low temperature gaz crossed by a continuous light absorbs some photons. Spectra then shows dark lines in front of the continuous spectra;
Emission line spectra: a low pressure high temperature gaz emits a light made of few radiations, characteristics of the atoms that constitutes this gaz. Each chemical element has its own line spectra, true identity card of its composition and state.
1
2
3
1
2
3
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Absorption lines ?
Sirius Spectrum – Buthier workshop 2007
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15/04/11 (c) 2006 - Shelyak Instruments 20
Low-resolution Solar SpectrumH
/ K
(Cal
cium
) Hδ
Hβ
Hα
Dou
blet
du S
odiu
m
Trip
let
du M
agné
sium
Olivier Thizy – Janvier 2007Lhires III – 300tt/mm; Digital Rebel / EOS300DPic du Midi (ie: no atmospheric lines!)
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Photospheric lines
D'après: http://ircamera.as.arizona.edu/astr_250/Lectures/Lecture_14.htm
• The photosphere is actually very thin
• The « wings » of spectral lines come from deeper layers than the « core »
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Absorbtion/Emission lines
∆Energy = h * ν = h *c / λ
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Table of elements
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Absorption lines
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Kirchhoff's laws
A continuous spectra is emitted by any solid of gazeous body under high presure and high temperature. Stars are, under first approximation, like black body whose continuous spectra has a shape which depends on its surface temperature;
Absorption line spectra: a low pressure low temperature gaz crossed by a continuous light absorbs some photons. Spectra then shows dark lines in front of the continuous spectra;
Emission line spectra: a low pressure high temperature gaz emits a light made of few radiations, characteristics of the atoms that constitutes this gaz. Each chemical element has its own line spectra, true identity card of its composition and state.
1
2
3
1
2
3
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Planetary Nebulae
Spectre de M57 (C. Buil)
Forbidden linesNames 'nebulium' orginally !
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Planetary Nebulae
M57 spectrum (C. Buil; LISA, C9, QSI583, 70min)
Nebula continuous spectrum
Emission lines (nebula)
Central star spectrum
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15/04/11 (c) 2006 - Shelyak Instruments 28
Planetary NebulaeNGC6826 - blink nebula
NGC7662 - blue snow ball
AstroQueyras T62 f/15, Lhires III (300tt/mm), ST10e / Olivier Thizy & Jose Ribeiro
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Emission lines
• Calibration lamp (here: internal neon lamp of a Lhires III spectrograph) create emission spectra
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Kirchhoff's lawswrap up!
A continuous spectra is emitted by any solid of gazeous body under high presure and high temperature. Stars are, under first approximation, like black body whose continuous spectra has a shape which depends on its surface temperature;
Absorption line spectra: a low pressure low temperature gaz crossed by a continuous light absorbs some photons. Spectra then shows dark lines in front of the continuous spectra;
Emission line spectra: a low pressure high temperature gaz emits a light made of few radiations, characteristics of the atoms that constitutes this gaz. Each chemical element has its own line spectra, true identity card of its composition and state.
1
2
3
1
2
3
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Stellar classification➢Some pioneers: Lewis Rutherfurd (1816-1892), Angelo Secchi (1818-1878), William Huggins (1824-1910), Hermann Carl Vogel (1841-1907)➢A key work: Henry Drapper catalog from Harvard
➢Edward Pickering (1846-1919) and his team (of women!); created AAVSO➢Williama Fleming (1857-1911): type A...Q; 26000 spectra➢Antonia Maury (1866-1952): typeI...XX; first to put O type before A type in Flemming classication➢Annie Cannon (1863-1941)
➢“OBAFGKM” types➢sub-divisions (B0..9)➢~400000 spectra of her own !!!
A.J. Cannon
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15/04/11 (c) 2006 - Shelyak Instruments 32
Spectral Classification (Low Res.)
C8 – Lhires III (150tt/mm) – EOS 300D – 30 sec – no computer !
A0
Be
M5
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From ABC... to OBAFGKM !
Spectra by Benjamin Mauclaire; 12'' telescope + Lhires III (150 gr/mm) + KAF1600 camera
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Relative intensity per elements
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15/04/11 (c) 2006 - Shelyak Instruments 35
Spectral Classification (High Res.)
Sequence around Calcium triplet, near Infra-Red. © Christian Buil / Lhires III + Digital SLR
Oh-Be-A-Fine-Girl-Kiss-Me
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15/04/11 (c) 2006 - Shelyak Instruments 36
Spectral Classification (High Res.)
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Stellar classification➢1890: Drapper catalog of stellar spectra➢1911-1915:225300 stars reviewed by A.J. Cannon➢1918-1924: HD (Henry Drapper) catalog published➢1949: HDE: HD catalog extension➢1943: “Atlas of Stellar Spectra” by William Morgan, Philip Keenan, & Edith Kellman [MKK]
➢Spectral type from HD catalog (Temperature): OBAFGKM➢Introduced class of luminosity I...V
E. Pickering team (all women!) in 1913.
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Beginning of Astrophysics➢Ejnar Hertzsprung (1873-1967) & Henry Russell (1877-1957)➢Color/Luminosity (first published in 1911)
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Doppler-Fizeau Effect
=c
Expansion of galaxies=
red shift
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15/04/11 (c) 2006 - Shelyak Instruments 40
In summary...
Light from the stars gives us information on:• Their temperature [overall profile]• composition and physical conditions of
excitation and ionization (ie temperature) [visible lines]
• quantitative chemical composition (abundance), pressure, gravity [line intensity and shape]
• movements [Doppler effect]● radial velocity● rotation● expansion
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15/04/11 (c) 2006 - Shelyak Instruments 41Equipment
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How does a spectrograph works?
➢Dispersion can be done by a prism or a grating➢Slit is one key element for high resolution resolution➢Littrow: collimator = objective➢Professional astronomers also use 'echelle' spectrographswith cross dispersing
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15/04/11 (c) 2006 - Shelyak Instruments 43
Equipment
Discover spectroscopy:The Star Analyser is the simplier spectroscope, ideal to get startedin this field with limited budget
Share your passion:Lhires Lite visual spectroscope for public outreach
Study:Lhires III (high resolution) and LISA (low resolution) are exploration tool allowing pro/am collcollaboration
Professional:eShel is an off-the-shelf optical fibre fed echelle spectrograph for higher RV accuracy and productive spectroscopy
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15/04/11 (c) 2006 - Shelyak Instruments 44
Spectral Domain
ResolvingPower R
Resolution(500nm)
Slit RV Limit mag
eShel 430-710nm >10000 0.5 A 50µmF/6
50 m/s ~10
Lhires III Visual(window of
~10nm)
~17000with2400
gr/mmgrating
0.3 A 15-35µmF/10
~3 km/s
~9
LISA 390nm-1µm
600-1000 5 A 15-35µmF/5
n/a ~16
Star Analyser Visual ~100 50 A No slit n/a ~15
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15/04/11 (c) 2006 - Shelyak Instruments 45
Applications
eShel High level educationBright stars line profile (Be stars, pulsations...)Abundances, classificationSpectroscopic binaries & exoplanets
Lhires III (self) education with low / medium / high resolution modesStellar classificationBright stars line profile (Be stars, eps Aur, Wolf-Rayet, Slow Pulsating B stars, Herbig Ae/Be...)
LISA Education: lamp, classification, nebulae, galaxie redshift...Faint variable stars: cataclysmics, novae, mira...Comets classificationAsteroids classification...
Star Analyser Education: star temperature & classificationNovaeFaint variable starsSupernovae
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15/04/11 (c) 2006 - Shelyak Instruments 46
In practice: in the field
At the telescope(autoguiding)
Control room-spectrograph-calibration unit-PC & observer :-)
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From image to profile...
Diffuse objet spectrum (ex: sun)
Slit
Stellar 2D spectrum
Spectral profile
Calibrated spectral profile
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Educational projects
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15/04/11 (c) 2006 - Shelyak Instruments 49
Solar spectrum (visual)
(c) Robin Leadbeater
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15/04/11 (c) 2006 - Shelyak Instruments 50
Spectro-Heliography
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15/04/11 (c) 2006 - Shelyak Instruments 51
Neon
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15/04/11 (c) 2006 - Shelyak Instruments 52
Thorium-Argon
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15/04/11 (c) 2006 - Shelyak Instruments 53
Hydrogen lab lamp
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15/04/11 (c) 2006 - Shelyak Instruments 54
Helium lab lamp
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15/04/11 (c) 2006 - Shelyak Instruments 55
Iodine lab lamp
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15/04/11 (c) 2006 - Shelyak Instruments 56
Nitrogen lab lamp
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15/04/11 (c) 2006 - Shelyak Instruments 57
unknown street lamp
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15/04/11 (c) 2006 - Shelyak Instruments 58
Sodium street lamp
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15/04/11 (c) 2006 - Shelyak Instruments 59
Light pollution...not always human !
C9 + LISA + QSI583 (C. Buil)Some emission from NGC7000 nebula!
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15/04/11 (c) 2006 - Shelyak Instruments 60
Spectrum of the trees !!!
« Red Edge » / C. Buil ; C9 + LISA (IR mode) + QSI583
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15/04/11 (c) 2006 - Shelyak Instruments 61
Planets – methan bands
Jim Edlin – Lhires III (150gr/mm) / C14 / ST10
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15/04/11 (c) 2006 - Shelyak Instruments 62
Planets – methan bands
C. Buil – Lhires III (1200gr/mm) – Digital SLR, near IR region (Calcium Triplet)
Methan bands:-on Saturn-not on rings !
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15/04/11 (c) 2006 - Shelyak Instruments 63
Planet's rotation
Saturn:Shift = 7 pixels = 8,8 km/sPeriod of 10,6 h >> R = 107511 km
T 2= 42G m1m2
a3
=c
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15/04/11 (c) 2006 - Shelyak Instruments 64
Planet's rotation: Saturn
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15/04/11 (c) 2006 - Shelyak Instruments 65
Stellar Rotation: v.sin(i)
v.sin(i) = 330km/s
v.sin(i) = 0km/s
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15/04/11 (c) 2006 - Shelyak Instruments 66
Stellar Rotation: v.sin(i)
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15/04/11 (c) 2006 - Shelyak Instruments 67
Stellar Radial Velocities
SAO104807, Altair, & SAO112958
=c
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15/04/11 (c) 2006 - Shelyak Instruments 68
Spectroscopic binaries
Spectrogrammes de Beta Auriga (30 spectres sur 2006/2007) / O. Thizy et al.
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15/04/11 (c) 2006 - Shelyak Instruments 69
Spectroscopic binaries
Spectrogrammes de Beta Auriga (30 spectres sur 2006/2007) / O. Thizy et al.
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15/04/11 (c) 2006 - Shelyak Instruments 70
Spectroscopic binaries
Beta Aurigae – O. Thizy / P. Noyrez
0.2 0.4 0.6 0.8 1.0Phase
150
100
50
50
100Vitesse Radiale
Paramètres orbitaux Cette étude (VSpec) Cette étude (PeakFit) Nordström (1994)K1 (km.s-1) 106 ± 3 108 ± 3 107.75 ± 0.40K2 (km.s-1) 108 ± 3 110 ± 3 111.25 ± 0.40
M1/M2 0.98 ± 0.06 0.98 ± 0.06 0.97 ± 0.01Vγ (km.s-1) -20 ± 2 -21 ± 2 -17.0 ± 0.4
a.sin(i) (Rsol) 16.7 ± 0.5 17.1 ± 0.6 17.13 ± 0.04m1.sin3(i) (Msol) 2.02 ± 0.06 2.15 ± 0.06 2.19 ± 0.02m2.sin3(i) (Msol) 1.99 ± 0.06 2.11 ± 0.06 2.12 ± 0.02
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15/04/11 (c) 2006 - Shelyak Instruments 71
Planetary Nebulae
Hα
[NII]
Spectre de NGC2392, C11+Lhires III (600tt/mm) + Atik16(c) Robin Leadbeater/O.Thizy – stage spectro OHP 2007
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15/04/11 (c) 2006 - Shelyak Instruments 72
Diffuse Nebulae
[OIII]5007
[OIII]4959
Hα6563
[NII]6583
[NII]6548
Spectre de M42 - Lhires III (150tt/mm) + KAF1600 / Acquisition: Benjamin Mauclaire / Traitement: Olivier ThizyCf: http://bmauclaire.free.fr/astronomie/spectro/atlas/nd/m42/Image de M42: Olivier Garde & Adrien Viciana (CALA)
Hβ4861
HeI5876
HeI6678
Te=10933±174 K
Ne=2537±61 e-/cm3
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15/04/11 (c) 2006 - Shelyak Instruments 73
Interstellar lines
P Cygni spectrum - Jean-Noël Terry – Lhires III (2400 gr/mm)
Na (interstellar)
Na (envelop)
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15/04/11 (c) 2006 - Shelyak Instruments 74
Precise temperature measurements
Measuring Equivalent Width of HeI [λ4471] & HeII [λ4541] ==> precise spectral type
HD 47839: HeI [λ4471] = 0.799 et HeII [λ4541] = 0.533 ==> type = O8
eShel Shelyak Instruments echelle spectrograph (R~11000)T0.28m f/6.3; Observatoire de Haute Provence – 2009, february 27
HeI
[λ44
71]
HeI
I [λ4
541]
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15/04/11 (c) 2006 - Shelyak Instruments 75
Peculiar stars
eShel + C11
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15/04/11 (c) 2006 - Shelyak Instruments 76
Galaxies: M31
C9 / LISA / QSI583 (C. Buil)
•Missing some blue part (aged stars in central part of M31)•Halpha is less visible
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15/04/11 (c) 2006 - Shelyak Instruments 77
Galaxies: M31
C9 / LISA / QSI583 (C. Buil)
•Broader lines (M31 rotation ?)•Doppler shift ~-280km/s (M31 is moving toward us)
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15/04/11 (c) 2006 - Shelyak Instruments 78
Galaxies red shift
C9 / LISA / QSI583 (C. Buil)
∆λ = 108 A==> z=0.016
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15/04/11 (c) 2006 - Shelyak Instruments 79
Galaxies red shift
C9 / LISA / QSI583 (C. Buil)
z=0.026
z=0.028
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15/04/11 (c) 2006 - Shelyak Instruments 80
Some steps back...
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Oleron 2003➢The situation
➢Very few pro/am collaboration (but some, see Buil Be star atlas), done with custom designed spectrograph.
➢Oleron 2003➢AUDE/CNRS pro/am official school➢Preceedings book to be published soon➢Kick off for Lhires III design➢Kick off Spectro-L list➢Kick off ARAS website front-end
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La Rochelle: 2006➢Be Stars Spectra (BeSS) database kick off
➢Structuring spectra collection & archiving➢Defining a spectra file format (FITS based)
➢Workshop on Lhires III (AUDE first kits just received !)
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La Rochelle: 2009➢10000 amateur spectra in BeSS...➢Exoplanet newly observed: pushing the limits...➢Dozen of active amateur spectroscopists...
➢==>More professional astronomers looking for help and support from amateurs !
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OHP practical workshops➢2004, 2005, 2007, 2008, 2009, 2010: a growing interest ! International attendance.➢30-40 instruments, all with spectrographs !➢Different style
➢workshop Vs talks, need for some theory➢structured project Vs autonomous groups➢courses Vs star party
➢ … the optimal format is hard to find !
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OHP ambiance...
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15/04/11 (c) 2006 - Shelyak Instruments 86
Pro/Am projects
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15/04/11 (c) 2006 - Shelyak Instruments 87
Comets
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15/04/11 (c) 2006 - Shelyak Instruments 88
Asteroids classification
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15/04/11 (c) 2006 - Shelyak Instruments 89
exoplanets !
Christian Buil
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15/04/11 (c) 2006 - Shelyak Instruments 90
Exoplanet: tau Boo
The CCF is computed by using the spectral range 4400-6445 A (the Halpha line is excluded).The total velocity Doppler spectral amplitude shift represents only 1/25th part of the spectrograph resolution. The dataare collected between March 19-March 29, 2009.
Christian Buil
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15/04/11 (c) 2006 - Shelyak Instruments 91
Exoplanet: tau Boo
The final phase plot of Tau Boo (HD120136). The star is observed during 9 nights. The Doppler signature of planetary compagnon is clearly visible (the velocity error bar is estimated to +/-100 m/s).
Christian Buil
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15/04/11 (c) 2006 - Shelyak Instruments 92
Exoplanets: 4 done so far
Christian Buil / Valérie Desnoux / Michel Pujol / Olivier Thizy
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15/04/11 (c) 2006 - Shelyak Instruments 93
Variable stars in general !
Source: Getting the measure of the stars (WA Cooper & EN Walker)
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15/04/11 (c) 2006 - Shelyak Instruments 94
Novae
2500 km/s
50 Å
V1280 Sco
RS Oph
V4743 Sgr
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15/04/11 (c) 2006 - Shelyak Instruments 95
Novae
Source: Jim Edlin; Lhires III (1200 gr/mm) + ST10
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15/04/11 (c) 2006 - Shelyak Instruments 96
Symbiotic stars: V407 Cyg
Note: another star spectrum is closed to V407 Cyg spectrum...
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15/04/11 (c) 2006 - Shelyak Instruments 97
Symbiotic stars: CI Cyg
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15/04/11 (c) 2006 - Shelyak Instruments 98
RR Lyrae: seeing stars pulsating live !
C.Buil
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15/04/11 (c) 2006 - Shelyak Instruments 99
BW Vul: at the heart of a star !!!
Spectrogram of HeI/Sodium doublet of BW Vul(5min expoure, 60cm f/3.5 telescope at pic du Midi)
0.0
1.0
phas
e
587.562He I
588.995Na
589.592Na
λ (nm)
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15/04/11 (c) 2006 - Shelyak Instruments 100
Herbig Ae/Be stars
C.Buil
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15/04/11 (c) 2006 - Shelyak Instruments 101
P Cygni
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15/04/11 (c) 2006 - Shelyak Instruments 102
other Active Hot Stars: Rigel, Deneb
➢Ref: arXiv:1007.2095v1 : Time, spatial, and spectral resolution of the Halpha line-formation region of Deneb and Rigel with the VEGA/CHARA interferometer
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15/04/11 (c) 2006 - Shelyak Instruments 103
Wolf-Rayet
O.Thizy
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15/04/11 (c) 2006 - Shelyak Instruments 104
WR140
Jose Ribeiro
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15/04/11 (c) 2006 - Shelyak Instruments 105
WR140 / 2009 periastron
Rémy Fahed et al.
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15/04/11 (c) 2006 - Shelyak Instruments 106
WR140 / 2009 periastron
Rémy Fahed et al.: CIII 5696 flat top line as function of phase / excess emission (right)
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15/04/11 (c) 2006 - Shelyak Instruments 107
Eps Aurigae eclipse
Robin Leadbeater
• Eclipse every 27 years !!!• ~15 amateurs contributing• Over 130 spectra to date ?
F typestar ?~7000K2.7 Msol ?
B star ?~15000K5.9 Msol
Disk~500K
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15/04/11 (c) 2006 - Shelyak Instruments 108
Eps Aurigae eclipse : KI 7699 line
Robin Leadbeater (Lhires III), Bob Stencel• New absorption line appearing !
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15/04/11 (c) 2006 - Shelyak Instruments 109
Robin Leadbeater (Lhires III), Bob Stencel: Contour plot showing the evolutionof the 7699A neutral potassium line after removal of the interstellar componentseen outside eclipse. Coverage is 140 days before first contact to 100 daysafter predicted mid eclipse.
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15/04/11 (c) 2006 - Shelyak Instruments 110
Eps Aurigae eclipse : KI 7699 line
Robin Leadbeater, Bob Stencel• Disk structures in « rings » ?
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15/04/11 (c) 2006 - Shelyak Instruments 111
Eps Aurigae eclipse : Halpha line
Robin Leadbeater, Bob Stencel: Contour plot showing the evolution of the H alpha linefrom pre first contact to approximately 100 days after predicted mid eclipse.It is generated from 159 spectra from all observers.
A hidden emission componentAn emission componentappeared in the core of theH alpha line close to the restwavelength.
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15/04/11 (c) 2006 - Shelyak Instruments 112
eps Aurigae pro-am campaign➢Complementary photometry / spectroscopy campaign➢Over 600 spectra collected (and increasing) !
➢Contacts: Robert 'Bob' Stencel (Denver, USA) Jeff Hopkins (amateur; photometry lead) Robin Leadbeater (amateur; spectroscopy lead)
➢Publications:➢http://www.threehillsobservatory.co.uk/astro/spectra_40.htm➢arXiv:0807.2855v1 : Gearing Up for Epsilon Aurigae's First Eclipse of the Millennium➢2009SASS...28..157H : Epsilon Aurigae Hydrogen Alpha Emission Line Variation: The Horn Dance➢2009CBET.1885....1W : Epsilon Aurigae (first detection !)➢arXiv:1003.3617v2 : Structure in the disc of epsilon Aurigae: Spectroscopic observations of neutral Potassium during eclipse ingress➢arXiv:1101.1435v1 : The International Epsilon Aurigae Campaign 2009-2011. A description of the campaign and early results to May 2010➢Article in Sky & Telescope magazine !
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15/04/11 (c) 2006 - Shelyak Instruments 113
A state-of-the-art pro/am project: Be stars
Hα
Pashen lines !!!
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15/04/11 (c) 2006 - Shelyak Instruments 114
Be stars
zet Tau
23 Tau
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Hα - time evolution β Lyr
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15/04/11 (c) 2006 - Shelyak Instruments 116
Exemple of Be targets: υ Sgr
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15/04/11 (c) 2006 - Shelyak Instruments 117
COROT targets: 64 Ser
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15/04/11 (c) 2006 - Shelyak Instruments 118
BeSS database
URL: http://basebe.obspm.fr
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15/04/11 (c) 2006 - Shelyak Instruments 119
BeSS catalog
● Plenty of BRIGHT stars to work on !!!F. Cochard / V. Desnoux
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15/04/11 (c) 2006 - Shelyak Instruments 120
BeSS database
● >11000 amateur spectra from over 30 different users
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15/04/11 (c) 2006 - Shelyak Instruments 121
Equipment used
TypeLhires III 42Pro 13Other 6eShel 5Total Résultat 66
● Amateur telescope size: 12cm to 62cm● Mainly Lhires spectrographs used by amateurs● eShel echelle spectrograph is new
but provides larger spectral coverage
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15/04/11 (c) 2006 - Shelyak Instruments 122
ArasBeAm “amateur” front end
http://arasbeam.free.frhttp://arasbeam.free.fr
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15/04/11 (c) 2006 - Shelyak Instruments 123
ARAS BeAm « to do » list
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15/04/11 (c) 2006 - Shelyak Instruments 124
ArasBeAm: detecting outburst
several outbursts
discovered
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15/04/11 (c) 2006 - Shelyak Instruments 125
delta Sco : 2011 periastron !!!
•Be stars identified as such in 1993•Outburst in 2000 with sudden increqse of visual brightness
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15/04/11 (c) 2006 - Shelyak Instruments 126
delta Sco : 2011 periastron !!!
Ernst Pollmann Tango et al. 2009
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15/04/11 (c) 2006 - Shelyak Instruments 127
delta Sco : 2011 periastron !!!
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15/04/11 (c) 2006 - Shelyak Instruments 128
delta Sco : 2011 periastron !!!
• Exact periastron date unknown (around beginning of July 2011)• Radial Velocity will change drastically few weeks before• Monitoring of H alpha is key• Monitoring of He I 6678 is very interesting too
==> amateur Spectroscopy is required !!!
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15/04/11 (c) 2006 - Shelyak Instruments 129
Telegram... from this morning !
Dear colleagues !Myron Smith, Computer Sciences Corporation, Space Telescope ScienceInstitute and my mentor in issues of gamma Cas, is asking for Halpha-EWobservations during the coming observation season.He and his colleague Greg Henry are very interested in correlationbetween Halpha-EW and photometric brightness within the UBV-system.Meanwhile they monitored the star in this way for 13 years (see fig. 3).Actually, I gave him the attached compiling plots (fig. 1 & 2) ofHalpha EW and visual brightness observations of my colleaguesin Hungaria and Germany.It would be great, if interested observers could measure the Halpha EWfor the coming months of visibility.Ernst Pollmann--------------------------------Active Spectroscopy in Astronomyhttp://www.astrospectroscopy.de ==> mag 2 star !
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15/04/11 (c) 2006 - Shelyak Instruments 130
ProAm projects overview
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in summary...• Spectroscopy reveal hidden details from the stars• Equipment is available off-the-shelf• Educational projects are numerous and fun • Pro/Am collaboration is increasing with more amateur contributing with more professionals requesting support
==> join us !!!
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Some useful links
Groupe ARAS: http://www.astrosurf.com/aras/
Liste Spectro-L: http://groups.yahoo.com/group/spectro-l/
SAS: http://www.socastrosci.org/
CDS Strasbourg http://cdsweb.u-strasbg.fr/
ADS (articles) http://adsabs.harvard.edu/abstract_service.html
Shelyak Instruments http://www.shelyak.com/
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Thank You !!!
Shelyak InstrumentsTél.: +33.476.41.36.81http://www.shelyak.comEmail: [email protected]