June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR Jason Kalirai (STScI) June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Outline - Frontier science opportunities for JWST in the arena of resolved stellar populations. - Characteristics of JWST that will enable this science. - Some hints from Hubble. - Synergies with HST, LSST, and GSMT.

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Carina Nebula - NASA, ESA, N. Smith (UC Berkeley), and the Hubble Heritage Team (STScI/AURA) Hubble Space Telescope ACS/WFC - STScI-PRC07-16A Resolved Stellar Populations in the Near IR Science Opportunities 1.) Calibrate the infrared color-magnitude diagram. 2.) Increase the sensitivity of main-sequence turnoff fitting methods. 3.) Complete the stellar inventory. 4.) Resolve distant galaxies into individual stars. June 07 th, 2011 Frontier Science Opportunities with JWST - STScI JWST Characteristics 1.) Superb sensitivity at near-infrared wavelengths. 2.) Multiple imaging and spectroscopic modes with fine sampling. 3.) High spatial resolution. 4.) Large fields of view.

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR 100 microns10 microns 1 microns Wavelength Light gathering power 0.1 microns (Mirror Area) HST JWST Spitzer Light Gathering Power JWST = 25 m 2 ; Hubble = 4.5 m 2 ; Spitzer = 0.6 m 2

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR JWST Sensitivity and Imaging Modes (see poster by J. Rigby)

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Hubble (D = 2.4 M) 0.5  m = 0.043’’ 1.6  m = 0.138’’ Diffraction Limits of Hubble, Spitzer, and JWST at various wavelengths (Minimum angular separation of a source that can be resolved) Spitzer (D = 0.8 M) 3.6  m = 0.93” 8.0  m = 2.06” 24  m = 6.18” JWST (D = 6.5 M) 2  m = 0.063’’ 4  m = 0.126’’ 10  m = 0.317’’ 20  m = 0.635’’ But, Hubble pixels are 0.04 – 0.05” at 1  m Spitzer pixels are 1.2” at <8  m and 2.55” at 24  m Hubble can not fully sample diffraction limit at optical or IR wavelengths Spitzer only reaches diffraction limit at > 24 microns JWST NIRCam has two modules, with pixel size ” at 2.5  m JWST MIRI has pixel size of 0.11 arcsec JWST optimally samples the diffraction limit at 2  m, 4  m, and 7+  m Best sampling demands a pixel size that is slightly finer than nyquist limit ( /2D) (i.e., ~2 pixels should sample the diffraction limits given above) Diffraction Limits Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI JWST Instruments: Imaging/Spectroscopic Modes and Fields of View The Near Infrared Camera (NIRCam) - Visible and near infrared camera (0.6 – 5 micron) x 4.4 arcmin field of view, diffraction limited The Near Infrared Spectrograph (NIRSpec) - Multi-object dispersive spectrograph (1 – 5 micron) x 3.4 arcmin field of view with 0.1 arcsec pixels - R = 1000 and 2700 gratings and R = 100 prism The Mid Infrared Instrument (MIRI) - Mid-infrared camera and slit spectrograph (5 – 28 microns) x 1.4 arcmin imaging field of view with 0.11 arcsec pixels - R = 100 slit spectrograph (5 – 10 micron) and IFU (R = 3000) The Tunable Filter Imager (TFI) - Selectable R = 100 tunable filters for imaging (1.5 – 5 micron) x 2.2 arcmin field of view NIRCam NIRSpec Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved stellar populations anchor our knowledge of the Universe JWST Opportunity #1: Calibrate the infrared color-magnitude diagram.

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR June 07 th, 2011 Frontier Science Opportunities with JWST - STScI

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR - NIRSpec can be extremely effective at obtaining large (~10,000 stars) statistical samples of stellar spectra in dense fields. Depending on density, 10-40% of all stars can be recovered. - This technique is very efficient because it can be done by reconfiguring the MSA only, without dithering. Sky background exposures are obtained “for free”. - This technique could be employed in globular clusters, star forming regions, the Galactic disk, and the bulge - provided the user requires a statistical sampling of stars. + Targets in operable shutter x Targets outside shutters NIRSpec MSA in Dense Stellar Fields Jason Tumlinson & Jay Anderson

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved stellar populations anchor our knowledge of the Universe JWST Opportunity #1: Calibrate the infrared color-magnitude diagram. Leads to better calibration of stellar evolution models at red wavelengths. Leads to smaller uncertainties in population synthesis models. Provides an improved interpretation of light from distant galaxies. Resolved Stellar Populations in the Near IR June 07 th, 2011 Frontier Science Opportunities with JWST - STScI

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Star clusters are excellent tracers of parent population star formation histories JWST Opportunity #2: Increase the sensitivity of main-sequence turnoff fitting methods. Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Sandage (1953) Buonanno et al. (1994) The Color-Magnitude Diagram Messier 3 (Photographic plates from 200”) Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI The Milky Way’s Globular Clusters M80NGC 2808 M55 NGC 6397M92Omega Cen Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI The Milky Way’s Globular Clusters Resolved Stellar Populations in the Near IR The Current State of the Art The HST/ACS Survey of Galactic Globular Clusters (Sarajedini et al. 2007) - Homogenous photometry and reduction. - V and I optical filters. - Modeled consistently with updated physics. - Large sample of 60+ clusters.

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR The Current State of the Art The HST/ACS Survey of Galactic Globular Clusters (Sarajedini et al. 2007) - Homogenous photometry and reduction. - V and I optical filters. - Modeled consistently with updated physics. - Large sample of 60+ clusters. NGC Dotter et al. (2010) Dotter et al. (2010)

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Main-Sequence Turnoff Fitting JWST Offers - Well separated filters in. - Superb sensitivity. - Larger field of view. - Diffraction limited. Transform current optical survey to panchromatic study. Calibration and tests of stellar evolution models into the IR. More sensitive mapping of star formation spreads. Resolved Stellar Populations in the Near IR T. Brown (priv communication)

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Star clusters are excellent tracers of parent population star formation histories JWST Opportunity #2: Increase the sensitivity of main-sequence turnoff fitting methods. Provides opportunity to probe <0.5 Gyr relative age spreads in clusters. Establishes more sensitive absolute age diagnostics. Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Co-spatial populations are excellent hunting grounds JWST Opportunity #3: Complete the stellar inventory. Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Based on HST/ACS and HST/WFC3 Data Collected as a Part of GO (PI H. Richer) UBC: Harvey Richer AMNH: Mike Shara, David Zurek HIA/NRC: Greg Fahlman, Peter Stetson Swinburne: Jarrod Hurley STScI: Jay Anderson, Aaron Dotter UBC: Jeremy Heyl, Ryan Goldsbury, Kristen Woodley UCLA: Brad Hansen, Mike Rich, David Reitzel UW: Ivan King Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR ACS/WFC visible color-magnitude diagram

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR WFC3/IR color-magnitude diagram

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR WFC3/UVIS and IR color-magnitude diagrams (1 HST orbit per filter)

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Resolved Stellar Populations in the Near IR A panchromatic data set: The color-magnitude relation

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Co-spatial populations are excellent hunting grounds JWST Opportunity #3: Complete the stellar inventory. Measure the initial mass function and its dependency on environment. Characterize the hydrogen burning limit and probe sub-stellar regimes. Resolved Stellar Populations in the Near IR

Apr 04 th, 2011University of British Columbia Brown et al. (2003) Field (126 HST/ACS Orbits) Resolved Stellar Populations in the Near IR Ultra-deep imaging JWST Opportunity #4: Resolve distant galaxies into individual stars.

Apr 04 th, 2011University of British Columbia Resolved Stellar Populations in the Near IR Brown et al. (2003) m F606W – m F814W

M31 N185 N147 M33 N205 M31 dSphs 30 kpc90 kpc150 kpc PAndAS M31 Map (McConnachie et al.) 60 kpc N E

SPLASH Project Collaborators UCSC: Raja Guhathakurta Caltech: Evan Kirby Cambridge: Andreea Font Columbia: Kathryn Johnston Japan: Masashi Chiba & Mikito Tanaka STScI: Tom Brown UC Irvine: James Bullock, Joe Wolf, Erik Tollerud UCSC: Kirsten Howley, Claire Dorman UMass: Mark Fardal UVa: Steve Majewski, Ricky Patterson, Rachael Beaton UW: Karrie Gilbert Yale: Marla Geha Resolved Stellar Populations in the Near IR

Apr 04 th, 2011University of British Columbia Observational Design - Keck II 10 meter telescope (on Mauna Kea) - DEIMOS spectrograph (R = 6000, FOV = 16’ x 4’, l = 6000 – 9000 Ang, # = 200 stars) Resolved Stellar Populations in the Near IR

Apr 04 th, 2011University of British Columbia Observational Design - Keck II 10 meter telescope (on Mauna Kea) - DEIMOS spectrograph (R = 6000, FOV = 16’ x 4’, l = 6000 – 9000 Ang, # = 200 stars) Resolved Stellar Populations in the Near IR Recent Results (SPLASH + PAndAS + Other) - Discovered M31’s stellar halo and measured its SB (Guhathakurta et al. 2006; Irwin et al. 2006) - Measured the spatial extent of the halo - R > 150 kpc (Gilbert et al. 2006; Ibata et al. 2007)

Apr 04 th, 2011University of British Columbia Observational Design - Keck II 10 meter telescope (on Mauna Kea) - DEIMOS spectrograph (R = 6000, FOV = 16’ x 4’, = 6000 – 9000 Ang, # = 200 stars) Resolved Stellar Populations in the Near IR Recent Results (SPLASH + PAndAS + Other) - Discovered M31’s stellar halo and measured its SB (Guhathakurta et al. 2006; Irwin et al. 2006) - Measured the spatial extent of the halo - R > 150 kpc (Gilbert et al. 2006; Ibata et al. 2007) - Characterized the halo metallicity distribution function (Kalirai et al. 2006; Chapman et al. 2006)

Apr 04 th, 2011University of British Columbia Observational Design - Keck II 10 meter telescope (on Mauna Kea) - DEIMOS spectrograph (R = 6000, FOV = 16’ x 4’, = 6000 – 9000 Ang, # = 200 stars) Resolved Stellar Populations in the Near IR Recent Results (SPLASH + PAndAS + Other) - Discovered M31’s stellar halo and measured its SB (Guhathakurta et al. 2006; Irwin et al. 2006) - Measured the spatial extent of the halo - R > 150 kpc (Gilbert et al. 2006; Ibata et al. 2007) - Characterized the halo metallicity distribution function (Kalirai et al. 2006; Chapman et al. 2006) - Discovered and characterized new substructures (Ibata et al. 2007; McConnachie et al. 2009; Kalirai et al. 2006; Gilbert et al. 2007; 2009a; 2009b; Fardal et al. 2007; 2008; 2009; Guhathakurta et al. 2006) - Measured the SFH in M31’s disk, spheroid, and stream (Brown et al. 2003; 2005; 2007; 2008)

Apr 04 th, 2011University of British Columbia Future Observational Design in for Samples of Galaxies - LSST wide-field imaging (substructure) - GSMT spectroscopy (kinematics, abundances) - JWST ultradeep imaging (SFHs) Resolved Stellar Populations in the Near IR - A view of the nearby universe, with galaxies at their true distances. Concentric circles correspond to hypothetical observing programs of 10, 100, and 1000 hours. - At a given distance, JWST will be nearly six times faster than HST for this type of work. - For a given exposure time, JWST can explore galaxies about 50% further away than those available to HST. T. Brown (priv communication)

Apr 04 th, 2011University of British Columbia Resolved Stellar Populations in the Near IR Ultra-deep imaging JWST Opportunity #4: Resolve distant galaxies into individual stars. Enable direct age measurements for components of samples of galaxies.

June 07 th, 2011 Frontier Science Opportunities with JWST - STScI Carina Nebula - NASA, ESA, N. Smith (UC Berkeley), and the Hubble Heritage Team (STScI/AURA) Hubble Space Telescope ACS/WFC - STScI-PRC07-16A Resolved Stellar Populations in the Near IR Science Opportunities 1.) Calibrate the infrared color-magnitude diagram. 2.) Increase the sensitivity of main-sequence turnoff fitting methods. 3.) Complete the stellar inventory. 4.) Resolve distant galaxies into individual stars. June 07 th, 2011 Frontier Science Opportunities with JWST - STScI