hubble’s slitless spectroscopy
DESCRIPTION
Hubble’s Slitless Spectroscopy. Patrick McCarthy – Carnegie Observatories. Hubble’s Slitless Spectroscopy. Slitless Spectra Stars & Planets Super Novae Faint Galaxies in the Visible Star forming & Passive systems Distant Galaxies in the Near-IR - PowerPoint PPT PresentationTRANSCRIPT
Hubble’s Slitless Spectroscopy
Patrick McCarthy – Carnegie Observatories
HST III Venice, October 2010 1
Hubble’s Slitless Spectroscopy
HST III Venice, October 2010 2
• Slitless Spectra
• Stars & Planets
• Super Novae
• Faint Galaxies in the VisibleStar forming & Passive systems
• Distant Galaxies in the Near-IR
See poster by H. Atek & talk by A. Straughn
• Slitless Spectra
• Stars & Planets
• Super Novae
• Faint Galaxies in the VisibleStar forming & Passive systems
• Distant Galaxies in the Near-IR
See poster by H. Atek & talk by A. Straughn
Slitless Spectroscopy
No entrance aperture - Disperser, PSF & Object shape set resolution- Focal plane image is a stack of
monochromatic images of all objects- No unique mapping between x,y and λ - Good software is essential!
No entrance aperture - Disperser, PSF & Object shape set resolution- Focal plane image is a stack of
monochromatic images of all objects- No unique mapping between x,y and λ - Good software is essential!
SN 1987A
Hα[NII][NII] [SII]
HST III Venice, October 2010 3
Slitless Spectroscopy
Backgrounds & Foregrounds – - All pixels see the full background- Wider band-pass more background- Background is dispersed and reintegrated, so higher
dispersion less contrast - Low dispersion is preferred
Backgrounds & Foregrounds – - All pixels see the full background- Wider band-pass more background- Background is dispersed and reintegrated, so higher
dispersion less contrast - Low dispersion is preferred
Best Targets:Compact objects with strong features
Cool stars, Planets, SNe, Distant Galaxies, AGN
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Slitless Spectroscopy
Good software is essential“AxE” package developed by ECF in Garching
- Background removal- Image plane – Spectral plane mapping- Spectral extraction, wavelength calibration and flat-fields
ECF Archive- NICMOS slitless grism spectra - 48,000 calibrated ACS slitless spectra
Good software is essential“AxE” package developed by ECF in Garching
- Background removal- Image plane – Spectral plane mapping- Spectral extraction, wavelength calibration and flat-fields
ECF Archive- NICMOS slitless grism spectra - 48,000 calibrated ACS slitless spectra
HST III Venice, October 2010 5
Two-Day Workshop on Slitless Grism Spectroscopy with Hubble
STScI - November, 15-16 See STScI website for details
Grisms for Slitless Modes on HST
R is 2-pixel resolution for point source
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Water Ice in the outer Solar System
HST III Venice, October 2010 7
Pluto Charon
NICMOS G141 & G206 Spectra
Exoplanet Atmospheres
NICMOS G141 & G206 Spectra of Exoplanet eclipse
HST III Venice, October 2010 8
Swain, Tinetti et al. Nature
High Redshift SNe Spectroscopy
ACS G800L spectra of
type Ia SNe to z ~ 1
Blakeslee et al. 2003
ACS G800L spectra of
type Ia SNe to z ~ 1
Blakeslee et al. 2003
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ACS Grism Spectroscopy
ACS G800L spectra of
Faintest Lyman Break
galaxies at z ~ 5
Rhoads et al. 2009
“GRAPES”
ACS G800L spectra of
Faintest Lyman Break
galaxies at z ~ 5
Rhoads et al. 2009
“GRAPES”
HST III Venice, October 2010 10
ACS Grism Spectroscopy
ACS G800L spectra of
Passive Galaxies in the UDF
Daddi et al. 2005
ACS G800L spectra of
Passive Galaxies in the UDF
Daddi et al. 2005
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NICMOS Grism Spectra
HST III Venice, October 2010 12
NICMOS G141 spectra of Hα emitters
1 – 3 orbits per frame
NICMOS G141 spectra of Hα emitters
1 – 3 orbits per frame
McCarthy et al. ‘99
1 emission line in every 3rd frame
1 line per object, max!
1 emission line in every 3rd frame
1 line per object, max!
Hα Luminosity Functions
Yan et al. 99, Hopkins et al. 2000, Shim et al. 2009
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Hα Luminosity Density
Shim et al. 2009HST III Venice, October 2010 14
Cycle 17 WFC3 Grism Programs
ERS Amber Straughn Pathfinder1 Field in both G102 & G141 GOODS-S2 orbits each
GO1161 Ben Weiner 56 orbits G141 in GOODS North 25 pointings, 2-orbits each
WISPS Matt Malkan “Wide-Field Infrared Spectroscopic Parallel Survey”
250 pure parallel orbitsG102 & G141 ~60 pointings 150 sq.
arcminutes1-5 orbits each grism
To Date: 40 pointings over 100 square arcminutes
ERS Amber Straughn Pathfinder1 Field in both G102 & G141 GOODS-S2 orbits each
GO1161 Ben Weiner 56 orbits G141 in GOODS North 25 pointings, 2-orbits each
WISPS Matt Malkan “Wide-Field Infrared Spectroscopic Parallel Survey”
250 pure parallel orbitsG102 & G141 ~60 pointings 150 sq.
arcminutes1-5 orbits each grism
To Date: 40 pointings over 100 square arcminutes
HST III Venice, October 2010 15
Zero-Order 1st-Order 2nd-Order
Emission-lines
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WFC3: 30 – 40 emission-line galaxies per field
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Star Forming Galaxies
[HeI]10830
[SIII]
WFC3 G102 + G141
2 orbits each
Atek et al. 2010
Same telescope,
same ruling (G141)!
z ~ 1
HST III Venice, October 2010 18
Star Forming Galaxies
[OIII]5007 is the strongest line, [OII]3727 is unimpressive
Atek et al. 2010
1.5 < z <2
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Star Forming GalaxiesNote numerous Hβ detections –
essential to E(B-V) and [Fe/H] determinations
Atek et al. 2010
High Equivalent Widths
[OIII] Hα
HST III Venice, October 2010 20
See Atek et al. poster
High Equivalent Widths
HST III Venice, October 2010 21
Rest-frame Wλ([OIII]) > 500A!
Keck/Deimos spectra of
z = 0.7 High EW
[OIII] emitter from G141
Keck/Deimos spectra of
z = 0.7 High EW
[OIII] emitter from G141
Redshifted “Green Peas”
“Red Beans”?
High Equivalent Widths
HST III Venice, October 2010 22
Sampling the Galaxy Mass Function
The WFC3 Grisms have the sensitivity to sample 0.1L* and fainter galaxies to
z > 2
Emission-line corrections push
continuum 1-2 mag fainter in some
cases
The WFC3 Grisms have the sensitivity to sample 0.1L* and fainter galaxies to
z > 2
Emission-line corrections push
continuum 1-2 mag fainter in some
cases
HST III Venice, October 2010 23
Quenched Galaxies at z = 1.5-2
Van Dokkum & Bremer 2010 Atek, Malkan, McC et al. 2010
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1 magnitude fainter!
500 Myrs after quenching of star formation
Quenched Galaxies at z > 2
Scarlatta, PMcC et al. 2010
Contamination
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Another magnitude fainter!
Passive Galaxies at z = 1 - 3
Scarlatta, PMcC et al. 2010HST III Venice, October 2010 26
G102 Search for Lyα Emission
Lyα at z = 6.8?
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Lyα?
Decrement?
H ~ 25AB
Cycle 18 & Beyond
“WISPS” Malkan et al. 280 pure parallel orbits
“3DHST” van Dokkum et al.248 prime orbits - G141 over full CANDELS area
2-orbit depth - Built on deep imaging fields
“CANDLES” & “CLASH” SNe grism spectroscopy
A slitless Deep or Ultra-Deep Field?
JWST 2-5μm slitless mode Hα to z = 6.5
Dedicated Slitless Missions – Euclid!
“WISPS” Malkan et al. 280 pure parallel orbits
“3DHST” van Dokkum et al.248 prime orbits - G141 over full CANDELS area
2-orbit depth - Built on deep imaging fields
“CANDLES” & “CLASH” SNe grism spectroscopy
A slitless Deep or Ultra-Deep Field?
JWST 2-5μm slitless mode Hα to z = 6.5
Dedicated Slitless Missions – Euclid!
HST III Venice, October 2010 28
HST III Venice, October 2010 29
Special Thanks to the ECF team for their dedicated effort to support slitless spectroscopy!
Richard Hook Jeremy Walsh Jonas Haase Harald Kuntschner Piero Rosati Martin Kornmesser Martin Kummel Marco Lombardi Kim Nilsson Brit Sjoberg Felix Stoehr Michael Rosa Colleen Sharkey Nor Pirzkal*
Special Thanks to the ECF team for their dedicated effort to support slitless spectroscopy!
Richard Hook Jeremy Walsh Jonas Haase Harald Kuntschner Piero Rosati Martin Kornmesser Martin Kummel Marco Lombardi Kim Nilsson Brit Sjoberg Felix Stoehr Michael Rosa Colleen Sharkey Nor Pirzkal*
And……
Bob Fosbury!
So Long, and Thanks for All the FishSpect
ra!
HST III Venice, October 2010 30