1. Hubble’s Slitless Spectroscopy Patrick McCarthy – Carnegie Observatories HST III Venice, October 20101

2. Hubble’s Slitless Spectroscopy HST III Venice, October 20102 Slitless Spectra Stars & Planets Super Novae Faint Galaxies in the Visible Star 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 Visible Star forming & Passive systems Distant Galaxies in the Near-IR See poster by H. Atek & talk by A. Straughn

3. 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] [SII] HST III Venice, October 20103

4. 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 HST III Venice, October 20104

5. 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 20105 Two-Day Workshop on Slitless Grism Spectroscopy with Hubble STScI - November, 15-16See STScI website for details

6. Grisms for Slitless Modes on HST R is 2-pixel resolution for point source HST III Venice, October 20106

7. Water Ice in the outer Solar System HST III Venice, October 20107 PlutoCharon NICMOS G141 & G206 Spectra

8. Exoplanet Atmospheres NICMOS G141 & G206 Spectra of Exoplanet eclipse HST III Venice, October 20108 Swain, Tinetti et al. Nature

9. 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 HST III Venice, October 20109

10. 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 201010

11. 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 HST III Venice, October 201011

12. NICMOS Grism Spectra HST III Venice, October 201012 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 3 rd frame 1 line per object, max! 1 emission line in every 3 rd frame 1 line per object, max!

13. Hα Luminosity Functions Yan et al. 99, Hopkins et al. 2000, Shim et al. 2009 HST III Venice, October 201013

14. Hα Luminosity Density Shim et al. 2009 HST III Venice, October 201014

15. Cycle 17 WFC3 Grism Programs ERSAmber StraughnPathfinder 1 Field in both G102 & G141 GOODS-S 2 orbits each GO1161Ben Weiner 56 orbits G141 in GOODS North 25 pointings, 2-orbits each WISPSMatt Malkan “Wide-Field Infrared Spectroscopic Parallel Survey” 250 pure parallel orbits G102 & G141~60 pointings 150 sq. arcminutes 1-5 orbits each grism To Date:40 pointings over 100 square arcminutes ERSAmber StraughnPathfinder 1 Field in both G102 & G141 GOODS-S 2 orbits each GO1161Ben Weiner 56 orbits G141 in GOODS North 25 pointings, 2-orbits each WISPSMatt Malkan “Wide-Field Infrared Spectroscopic Parallel Survey” 250 pure parallel orbits G102 & G141~60 pointings 150 sq. arcminutes 1-5 orbits each grism To Date:40 pointings over 100 square arcminutes HST III Venice, October 201015

16. Zero-Order 1st-Order 2nd-Order Emission-lines HST III Venice, October 201016 WFC3: 30 – 40 emission-line galaxies per field

17. HST III Venice, October 201017 Star Forming Galaxies [HeI]108 30 [SIII] WFC3 G102 + G141 2 orbits each Atek et al. 2010 Same telescope, same ruling (G141)!

18. z ~ 1 HST III Venice, October 201018 Star Forming Galaxies [OIII]5007 is the strongest line, [OII]3727 is unimpressive Atek et al. 2010

19. 1.5 < z <2 HST III Venice, October 201019 Star Forming Galaxies Note numerous Hβ detections – essential to E(B-V) and [Fe/H] determinations Atek et al. 2010

20. High Equivalent Widths [OIII] Hα HST III Venice, October 201020 See Atek et al. poster

21. High Equivalent Widths HST III Venice, October 201021 Rest-frame W λ ([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”?

22. High Equivalent Widths HST III Venice, October 201022

23. 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 201023

24. Quenched Galaxies at z = 1.5-2 Van Dokkum & Bremer 2010 Atek, Malkan, McC et al. 2010 HST III Venice, October 201024 1 magnitude fainter! 500 Myrs after quenching of star formation

25. Quenched Galaxies at z > 2 Scarlatta, PMcC et al. 2010 Contamination HST III Venice, October 201025 Another magnitude fainter!

26. Passive Galaxies at z = 1 - 3 Scarlatta, PMcC et al. 2010 HST III Venice, October 201026

27. G102 Search for Lyα Emission Lyα at z = 6.8? HST III Venice, October 201027 Lyα? Decrement? H ~ 25AB

28. 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? JWST2-5μm 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? JWST2-5μm slitless mode Hα to z = 6.5 Dedicated Slitless Missions – Euclid! HST III Venice, October 201028

29. HST III Venice, October 201029 Special Thanks to the ECF team for their dedicated effort to support slitless spectroscopy! Richard HookJeremy WalshJonas Haase Harald KuntschnerPiero RosatiMartin Kornmesser Martin KummelMarco LombardiKim Nilsson Brit SjobergFelix StoehrMichael Rosa Colleen SharkeyNor Pirzkal* Special Thanks to the ECF team for their dedicated effort to support slitless spectroscopy! Richard HookJeremy WalshJonas Haase Harald KuntschnerPiero RosatiMartin Kornmesser Martin KummelMarco LombardiKim Nilsson Brit SjobergFelix StoehrMichael Rosa Colleen SharkeyNor Pirzkal* And…… Bob Fosbury! So Long, and Thanks for All the Fish Spectr a!

30. HST III Venice, October 201030