IRTF 김도형

Contents About IRTF Instruments on the IRTF -Introduction of instruments -Sciences from instrument What can we do with IRTF?

Contents About IRTF Instruments on the IRTF -Introduction of instruments -Sciences from instrument What can we do with IRTF?

About IRTF NASA InfraRed Telescope Facility 3.0 meter telescope, optimized for infrared observations 50% of the IRTF observing time is reserved for studies of solar system objects Located at the summit of Mauna Kea, Hawai`i

Subaru Keck IRTF

Atmosphere absorption a

About IRTF NASA InfraRed Telescope Facility 3.0 meter telescope, optimized for infrared observations 50% of the IRTF observing time is reserved for studies of solar system objects Located at the summit of Mauna Kea, Hawai`i

About IRTF Subaru 8.2m Keck 10m Gemini 8.1m UKIRT 4m CFHT 3.6m IRTF 3m

Contents About IRTF Instruments on the IRTF -Introduction of instruments -Sciences from instrument What can we do with IRTF?

Instruments on the IRTF SpeX: Micron Medium-Resolution Spectrograph and Imager CSHELL: μm high resolution single-order echelle spectrograph MIRSI: A Mid-Infrared Spectrometer and Imager (2-28 μm) MORIS: high-speed, visible wavelength imager & spectrograph

NIR Spectroscopy Instruments SpeX: μm CSHELL: MIRSI: 2-28 μm Subaru: COMICS- Cooled Mid-Infrared Camera and Spectrograph - provides imaging and spectroscopy from 8-25 microns Subaru: IRCS - Infrared Camera and Spectrograph - provides imaging from microns, and low-resolution and echelle spectroscopy over the same range Gemini: NIRI - 1-5µm imager with grism spectroscopy Gemini: MICHELLE µm imager/ spectrometer; imaging polarimetry Keck: NIRC - instrument designed to produce both infrared images and low resolution spectra from 1 to 5 µm Keck: NIRSPEC μm CFHT: ESPaDOnS Å to 10500Å UKIRT: X

MIRSI The two grisms cover μm at a resolution of up to 200 (using a 0.6'' slit), and μm range at a resolution of up to 100 (1.2'' slit) Filters for imaging consist of narrowband filters for both the 10 and 20 μm windows spatial resolution 10 microns at IRTF )

MIRSI’s Scientific Topic Star Formation Planetary Nebulae Starburst Galaxies Extra Solar System Solar System Body

Studies with MIRSI Test model of star formation process -The role of small dust grains and large molecules, such as PAH, and place constraints on the extent of the dust envelope -Mapping of entire molecular cloud complexes by MIRSI's wide field of view -> -Shock dynamics in circumstellar shell of embedded objects with high amounts of obscuration Identifying mid-IR properties of planet -To probe Jupiter's atmospheric properties using CH4 (7.8 microns), H2 (13.0 microns), and NH3 (10.74 and 8.57 microns, gas and ice).

Hoffmann et al microns image of the Orion Nebula, taken at IRTF Suitable equipment to study galactic star-forming regions such as these using both imaging and spectroscopy in the 10 and 20 micron atmospheric windows FOV = 85 x 64 arcsec MIRSI’s large field of view

Studies with MIRSI Test model of star formation process -The role of small dust grains and large molecules, such as PAH, and place constraints on the extent of the dust envelope -Mapping of entire molecular cloud complexes by MIRSI's wide field of view -> -Shock dynamics in circumstellar shell of embedded objects with high amounts of obscuration Identifying mid-IR properties of planet -To probe Jupiter's atmospheric properties using CH4 (7.8 microns), H2 (13.0 microns), and NH3 (10.74 and 8.57 microns, gas and ice).

SpeX medium-resolution μm spectrograph R~ across μm, μm, μm and μm (using cross disperser) prism mode is a provided for micron spectroscopy at R~100

SpeX Cross disperser Modes of SpeX

SXD Sample Red quasar z~0.7

Prism Sample High z quasar (z=6.04±0.01) Ly β Ly α SiIV CIV MgII

Prism Sample High z quasar (z=6.04±0.01) Ly β Ly α SiIV CIV MgII h0224 T~1500K Brown dwarf

Observing Schedule

Scientific Topic Dwarfs Solar system AGNs Molecular Cloud Supernovae

Dwarf Study with SpeX Discovery of ultra-cool brown dwarf T_eff=600K [Fe/H]=0 Mainzer et al. 2011

Resolved Spectroscopy of M Dwarf& L Dwarf Binaries Dhital et al. 2011

Resolved Spectroscopy of M Dwarf& L Dwarf Binaries Resolved spectroscopy of M dwarf& L dwarf by using IRTF’s various slit width (0.3, 0.5, 0.8, 1.6 and 3.0”)

Comet 17P/ Holmes Yang et al ??

Hot Dust Property of AGNs Hot dust temperature is ~1500K The power-law slope of AGNs was changed by the effect of hot dust BB radiation Glikman et al. 2006

Stellar& Dust Populations of Seyfert Galaxy A first approach of stellar& dust contamination study in NIR Riffel et al. 2011

The Existence of Red Shelf The FWHMs of Hβ are broader than those of Pβ Landt et al. 2008

The Paschen line BH mass estimator The BH masses estimated by Paschen line have a tight correlation with those of existed method Kim et al. 2010

H2O Ice in Dense Cloud Chiar et al. 2011

The NIR catalog of SN Marion et al. 2009

CSHELL Cryogenic Near-IR Facility Spectrograph μm high resolution single- order echelle spectrograph R Slit width (arcsec)

Hot Wind from T Tauri Star Fast and hot accelerating outflow from T tauri star Dupree et al. 2005

Molecular hydrogen gas of T tauri stars Weintraub et al. 2000

Studies of Solar System Evidence for a dominant native source of carbon monoxide in Comet C/1996 B2 (Hyakutake) – DiSanti et al Methane in Oort cloud comets – Gibb et al High-resolution spectroscopy of Venus: Detection of OCS, upper limit to H 2 S, and latitudinal variations of CO and HF in the upper cloud layer – Krasnopolsky 2008 Detection of Formaldehyde Emission in Comet C/2002 T7 (LINEAR) at Infrared Wavelengths: Line-by-Line Validation of Modeled Fluorescent Intensities – DiSanti et al …

Contents About IRTF Instruments on the IRTF -Introduction of instruments -Sciences from instrument What can we do with IRTF?

AGN-Starburst Connection Composite spectrum of PG QSO with the Subaru IRCS Kawakatu & Wada (2008) predicted that the nuclear-starburst to AGN luminosity ratio will increase with increasing AGN luminosity, whereas Ballantyne (2008) has argued the contrary Imanishi et al. 2011

Discovery of dwarf& high z (~6) QSO Ly β Ly α SiIV CIV MgII Mainzer et al. 2011

The Competition Rate of IRTF 2010A: 1.7 for solar system and 2.8 for non-solar system proposals 2010B: 1.7 for solar system and 2.1 for non-solar system proposals 8m Telescope: over than 5?? Space Telescope: over than 10??

The Competition Rate of IRTF 2010A: 1.7 for solar system and 2.8 for non-solar system proposals 2010B: 1.7 for solar system and 2.1 for non-solar system proposals 8m Telescope: over than 5?? Space Telescope: over than 10?? Mainzer et al. 2011

How to Submit? A season: February 1 – July 31 (10/1) B season: August 1 - January 31 (4/1) To prepare application by LaTex or Word