Infrared Astronomy in the heat of the night Michael Burton

Infrared Astronomy ◊What is the infrared ◊Infrared Science Imaging Spectroscopy ◊History and the Future ◊Infrared Movies ◊What is the infrared ◊Infrared Science Imaging Spectroscopy ◊History and the Future ◊Infrared Movies

William Herschel “Calorific Rays” in 1800

Infrared is Heat Thermal Radiation

Two views of a geyser

1.Dust Extinction Exploring the hidden universe Galactic CentreCygnu s

2. Thermal Radiation Detecting Cool Objects

3. Redshift Exploring the Early Universe

Atmospheric Windows

Infrared Windows

IR Observatories on the ground, in the air and in space

The Horsehead Nebula VisibleNear-IRMid-IR

Massive Star Formation Triffid Nebula

The Galactic Centre VisibleNear-IR

Three Spectral Regimes Detector Technology

Some infrared science ◊Solar System ◊Star Formation ◊Stars ◊Disks and Planets ◊Galaxies ◊Solar System ◊Star Formation ◊Stars ◊Disks and Planets ◊Galaxies

Venus Infrared emission vs. Visible reflection

Jupiter Bright belts, volcanic Io, methane absorption

Star Formation Orion Constellation Far-IR Dust Orion Nebula Near-IR Young Stars Nearby Globule Mid-IR Dust + Protostars

Massive Stars ◊Pistol Star Most luminous star in Galaxy ~10 7 L  ◊Quintuplet Cluster Most massive star cluster in Galaxy  Max mass of a star?

Dust Disks and Planets Beta Pictoris HR4796A

The Galaxy Near + mid-IR Galactic Centre Red Giants + Hot Dust Far--IR Galactic Plane Zodiacal Light + Warm Dust

Other Galaxies: Spiral M81 ◊Old Stars (blue) ◊Heated Dust (red) ◊Hot Dust and MSF (green + knots)

Global Star Formation Spiral Galaxy M51

Hidden Black Holes in the IR

Infrared Spectroscopy ◊Cooling Lines Molecules Fine structure lines ◊Ices ◊Dust ◊Cooling Lines Molecules Fine structure lines ◊Ices ◊Dust

Infrared Spectroscopy Water in the Solar System Hydrocarbons, Ices, Dust mineralology

Cooling Lines in the ISM [OI] 63µm + [CII] 158µm

Cooling Lines across the Galaxy [CII] 158µm + [NII] 205µm

Water and Ices in Molecular Clouds

Elements and Minerals in Red Giants and PN winds Recycling of the elements

Star Formation in the Galactic Centre Hot massive stars, ionized gas,  ~10 7 yrs

Molecules in Dusty Galaxies Spiral NGC891 Starburst Arp 220

Probing the Excitation of Galaxies

A potted history of IR astronomy 1800: William Herschel Discovery of IR 1948: Moon must be covered By fine powder 1870: 4th Earl of Rosse Temperature of Moon From IR on dark side 1856: Charles Piazzi IR from the Moon Thermocouple & heat

IR Facilities: the early days 1967: Mauna Kea Observatory established High & dry! 1967: Cooled IR telescopes in rockets AFGL IR sky survey µm 2363 sources in 30 mins 1960’s: Balloons carry high altitude payloads 1961: Frank Low Germanium bolometer Cooled, in dewar Detect far-IR Change in conductivity

IR Facilities Develop Mid 1970’s: Far-IR spectrometers from balloons at T = 1K CMBR Early 1970’s: Most galaxies found to emit strongly in IR (M31) 1974: Kuiper Airborne Observatory Rings of Uranus Water in Jupiter 1968: Leighton & Neugebauer Mt Wilson 2.2µm IR survey 5,500 sources

IR Facilities Mature 1989: COBE MM + Far-IR sky CMBR 1985: IR telescope on Shuttle 1983: IRAS satellite µm 500,000 sources Vega Disk ULIRGs 1980’s: IR arrays

IR in the 90s 1996: MSX Military satellite µm 1996: DENIS Near-IR sky survey La Silla, Chile 1995: ESA ISO µm + spectroscopy 1994: SPIREX at the South Pole

IR Astronomy Today 2004: Spitzer Space Telescope 2001: Keck Interferometer 1997: NICMOS on HST 1-2.5µm 1997: 2MASS All-sky µm

IR Astronomy Tomorrow 2???: TPF/Darwin Other Earths?! 2008?: Planck CMBR 2008?: Herschel - far-IR 2007?: SOFIA - IR spectroscopy

Infrared Astronomy for Australia ◊Siding Spring Observatory AAT/IRIS1-2.5µm Imager/Spectrometer 2.3m/CASPIR1-5µm Imager ◊Gemini 1-5µm NIFS µm Michelle / TReCS ◊Public Databases 2MASS (1-2µm), MSX (8-21µm), GLIMPSE (4- 8µm), IRAS (12-100µm) ◊Antarctica Finest ground-based sites on the Earth! ◊Siding Spring Observatory AAT/IRIS1-2.5µm Imager/Spectrometer 2.3m/CASPIR1-5µm Imager ◊Gemini 1-5µm NIFS µm Michelle / TReCS ◊Public Databases 2MASS (1-2µm), MSX (8-21µm), GLIMPSE (4- 8µm), IRAS (12-100µm) ◊Antarctica Finest ground-based sites on the Earth!

Dark Cloud + HH46-47 Optical to Infrared (Spitzer)

Dark Globule IC1396 Visible to Infrared (Spitzer)

Massive Star Formation Triffid: Visible to IR (Spitzer)

Spiral Galaxy M51 Visible to Infrared (Spitzer)

2MASS 1-2µm View Galactic Centre

MSX 8-21µm view of the Galaxy PAHs along the Milky Way

Eta Carina Star Forming Complex