ALMA: Im aging the co ld Univ e rs e C. Carilli (NRAO) National Research Council Canada AAS ALMA Town Meeting, Washington, DC 2006
(s ub)m m as tro no m y : unv e iling the co ld, o bs cure d univ e rs e SCUBA Wilson et al. Shirley et al. B335 DSS HST / OVRO CO
Giant Ste ps I: Fre que n cy and re s o lutio n
Giant Ste ps I: Fre que n cy and re s o lutio n 20mas at 0.9THz (300um)
Gian t Ste ps II: Se n s itiv ity Inde x= 1.7
Gian t Ste ps II: Se n s itiv ity Cu r r en t z> 2 5 e1 0 M_s u n Inde x= 1.7
Gian t Ste ps II: Se n s itiv ity Cu r r en t z> 2 ALMA Line: 0.1 mjy in z> 2 1 hr at 2 3 0 GHz Inde x= 1.7 1 e9 M_s u n 5 e1 0 M_s u n
Giant Ste ps III: Im age quality 5 0 + ant, ACA, TP Optical/ ESO IR/ ISO T_lin e = s u b- K at 0.25 arcsec res. T_con t = m K at 0.25 ar cs ec res. CO 3-2 / CSO
Giant Ste ps IV: Site quality 0.5 at 0.9 THz
Birth of s tars : phy s ics / che m is try of s tar fo rm atio n in 3 D Lin e con fu sion lim ited = > n ew m od e of op er ation : tar geted lin e s tu d ies Select lin es as p r ob es of: d en sity, tem p erat u r e, excit at ion, evolu tion ar y s tate, or d yn am ics Pu t s p res su r e on lab or at or y as tr op h ys ics, an d d at a an alys is / vis u aliz at ion S/ W
Birth o f plan e ts Mp lan et / Ms t ar = 1.0 MJu p /.5 Ms u n Orb it al r ad iu s : 5AU at 50p c d ist an ce Dis k m as s = cir cu m s t ellar d is k ar ou n d t h e Bu t ter fly Star in Tau r u s ALMA 850 GHz Williams + HST 5AU Wolf
Su b m m su rveys: Probin g t h e ep och of galaxy form at ion (z = 1.5 3) SCUBA 20 m Jy SMA/ Sp it z er HST 20mJy at 350 GHz Co m p a r a b le SFR a t z > 2 in d u s t y s t a r b u r s t s ( s u b m m ga l ) a s op t ica lly s elect ed ga la xies = for m a t ion of la r ge ellip t ica l ga la xies?
ALMA De ep fie ld: norm al galaxie s at high z HST Det ect cu r r en t s u b m m ga l in s econ d s! ALMA d eep s u r vey: 3 d a ys, 0.1 m Jy (5 σ), 4 HST: few 1 0 0 0 Ga l, m os t a t z < 1.5 z < 1.5 ALMA z > 1.5 ALMA: few 1 0 0 Ga l, m os t a t z > 1.5 Pa r a llel s p ect r os cop ic s u r veys, 1 0 0 a n d 2 0 0 GHz : CO/ o t h er lin es in m a jor it y of s ou r ces Red s h ift s, d u s t, ga s m a s s es, p lu s h igh r es. im a ges of ga s d yn a m ics, s t a r for m a t ion
SDSS J1 1 4 8 + 5 2 5 1 : Du s t a n d m olecu la r ga s in t o cos m ic r eion iz a t ion J1148 VLA: CO 3-2 z = 6.4 2 1 2.5 Fan + 1 e 9 M_s un in dus t, 1 e 1 0 M_s un in m ol. gas => [C II] [CII] Hyp er lu m in ou s IR galaxy (FIR = 1e13 L_su n ) : SFR = 1e3 M_su n / yr? CO CO6-6-5 5 Coeval for m at ion of SMBH/ Galaxy? Du s t for m at ion b y m as sive s tar s? Br eak- d own of M- σ r elation at h igh z? Ear ly en r ich m en t of h eavy elem en ts (z _sf > 8) IRAM In tegr ation t im es : h ou r s t o d ays on HLIRGs
ALMA in t o t h e EoR Spe ctral s im ulatio n o f J1 1 4 8 + 5 2 5 1 CO HCO+ HCN CCH Det ect d u s t em is s io n in 1 s e c (5 σ) a t 25 0 GHz Det ect m u lt ip le lin es, m o lecu les p er b a n d = > d et a iled a s t r o ch em is t r y Im a ge d u s t a n d ga s a t s u b - kp c r es o lu t io n ga s d yn a m ics! Stu dy in g 1 s t galax ie s Det ect n or m a l (eg. Ly α), s t a r for m in g ga la xies, like M51, a t z > 6, in few h ou r s Det er m in e r ed s h ift s d ir ect ly fr om m m s p ect r os cop y z = 6.55 SFR> 10 M_sun / yr SFR> 10M_su n / y r
ALMA p an ch rom at ic view of galaxy form at ion Ar p 2 2 0 vs z cm : Star fo rm atio n, AGN (s ub)m m Dus t, m o le cular gas Ne ar- IR: Stars, io niz e d gas, AGN
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Very wid e field s u r veys : r ole of bolom et er cam eras Bolo m et er s (+ EVLA, Sp it z er ): s u r vey la r ge a r ea s t o s u b m Jy s en s it ivit y ALMA: d et a iled SED a n d CO follow- u p ALMA: u Jy, n a r r ow field s u r veys
Sum m ary of detailed requirem ents Frequency 30 t o 950 GHz (init ially only 84-720 GHz) Bandwidt h 8 GHz, fully t unable Spect ral resolut ion 31.5 khz (0.01 km/ s) at 100 GHz Angular resolution 1.4 t o 0.015 at 300 GHz Dynamic range 10000:1 (spect ral); 50000:1 (imaging) Flux sensitivity 0.2 mjy in 1 min at 345 GHz (median conditions) Ant enna complement 64 ant ennas of 12m diamet er Polarization All cross product s simult aneously
UV s elect ed galaxies large ran ge in bolom et ric lu m in os it y, b u t lit t le correlat ion of L_u v an d L_bol Ade lbe rge r 2 0 0 0
Millim et er VLBI Im agin g t h e Galact ic cen t er black h ole (Falcke 2000) Ker r R_g = 3 uas Sch war z s ch il d Mode l: o pt. thin s y nch 0.6 m m VLBI 1.3 m m VLBI 1 6 uas re s 3 3 uas re s
Birth o f Galax ie s : Magic o f (s ub)m m L_FIR = 1.5 e12 L_s u n 1m Jy
SDSS J1148 + 5 25 1: Du s t an d m olecu lar gas in t o cos m ic r eion iz at ion 1 e 9 M_s un in Dus t, 1 e 1 0 M_s un in m ol. Gas = > Hyp er lu m in o u s IR galaxy (FIR= 1e13L_s u n ) Early en rich m en t o f h eavy elem en t s (z _s f > 10?) Du s t fo rm at io n b y m as s ive s t ars? M_d yn (r= 2.5 kp c) = 2.5 e10 M_s u n coeval for m at io n o f SMBH/ Galaxy? Break- d o wn o f M- σ relat io n at h igh z? In t egrat io n t im es : h o u rs t o d ays [C II] CO 65 CO 3-2 z = 6.4
Wilson et al. (s ub)m m as tro no m y : unv e iling the co ld, o bs cure d univ e rs e IR Optical IC34 2 Optical Infrared Shirley et al. France s chini 2000 Franceschini Co s m ic Back gro u n d Radiatio n