Wide Field Imaging for Nearby Galaxies
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1 Wide Field Imaging for Nearby Galaxies Hiroyuki Nakanishi (Kagoshima university) 2013/07/ EA ALMA Development Workshop 1
2 Next years of Radio Astronomy New large projects will start science operaqon SKA TMT SPICA /07/ EA ALMA Development Workshop 2
3 SKA (Square Kilometer Array) Freq.:50MHz-10GHz Antenna:15m-dishes x 3000 Max baseline: 3000km Site: Australia (low-ska) and South Africa (mid-ska) Characteristics High Sensitivity High Reslolution Wide Field of View Wide Band Width 2013/07/ EA ALMA Development Workshop 3
4 First concept of SKA in ASPC W 2013/07/ EA ALMA Development Workshop 4
5 Study of Nearby Galaxies in 10yrs Introductory material 1. MoQvaQon, key science projects, standards and assumpqons Key Science Projects 2. Cradle of Life 3. Strong- field tests of gravity using pulsars and black holes 4. The origin and evoluqon of cosmic magneqsm 5. Galaxy evoluqon, cosmology and dark energy with the Square Kilometre Array 6. Probing the dark ages with the Square Kilometre Array Science Chapters 27. HI imaging the low red- shi^ cosmic web R. Braun 30. ObservaQons of magneqc fields in the Milky way and in nearby galaxies with a Square Kilometre Array R. Beck, B. M. Gaensler 31. ISM in nearby galaxies - E. Brinks SKA Science Book /07/ EA ALMA Development Workshop 5
6 Next study for nearby galaxies Cosmic web MagneQc field Star FormaQon law HI- H2 transiqon 2013/07/ EA ALMA Development Workshop 6
7 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon 1. Cosmic Web Braun & Thilker 2004 IntergalacQc diffuse HI is being detected by unbiased HI survey Galaxies are not isolated, interacqng with others. SF history is affected Yun, Ho & Lo /07/ EA ALMA Development Workshop 7
8 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon 2. Cosmic magneqc field Morphology of magneqc field BSS, ASS or Ring VerQcal structure Coherency ObservaQonal test of galacqc dynamo process MagneQc field in low density region (halo and IGM) 2013/07/ EA ALMA Development Workshop 8
9 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon 3. Star- formaqon in low gas density and low metallicity GALEX observaqon: star- formaqon (SF) outside the opqcal disk. No molecular cloud detected yet. Important to understand SF in the primordial gas Thilker et al /07/ EA ALMA Development Workshop 9
10 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon SF in the GalacQc outer disk UBVI imaging of the outer Galaxy with Kiso Schmidt camera CC- diagram photometric distance of OB stars No cutoff detected in stellar density profile The Galaxy and galaxies seem to have larger SF disks than ever thought HN et al /07/ EA ALMA Development Workshop 10
11 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon Nobeyama Outer Galaxy Survey Searched for molecular clouds in the Outer Galaxy No clouds detected beyond R GC =15kpc (M min =40 Mo) - too large X CO? Ongoing project: GalacQc plane survey with FOREST. Next 10 years: Survey for molecular clouds in the outer disks of nearby galaxies. M.Matsuo, HN et al. in prep 2013/07/ EA ALMA Development Workshop 11
12 Cosmic web MagneQc field Star FormaQon law HI- H2 transiqon 4. HI- H2 transiqon H2 and HI are dominant in the inner and outer Galaxy, respecqvely. What determines fmol? fmol=σh2/(σh2+σhi) Crosthwaite et al /07/09 Honma et al EA ALMA Development Workshop 12
13 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon What determines f mol? Elemegreen 1993 P f mol U f mol Z f mol 8 (P/P0) dust 2013/07/ EA ALMA Development Workshop 13
14 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon Comparison of observaqon and theory f mol =σ H2 /(σ H2 +σ HI ) theory P, U, Z M51 σ H2+HI M51 Obs. I CO (obs) I HI (obs) I Hα (obs) O/H (obs) I K 2013/07/ EA ALMA Development Workshop 14
15 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon Some issues to be solved CalculaQon of P: Which is the best o? 1. P Σ tot (Honma et al., 1995) 2. P Σ 2 tot (Elmegreen, 1993) 3. P Σ tot Σ * (Blitz & Rosolowsky, 2004) X CO : constant or funcqon of metallicity? 1. X CO =α (cm - 2 (K km s - 1 ) - 1 ) (α = 1-3) 2. X CO = f ( log Z ) (Arimoto et al. 1996, Narayanan et al.,2012) 2013/07/ EA ALMA Development Workshop 15
16 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon Comparison of observaqon and theory If P Σ tot Σ * and X CO = (cm - 2 (K km s - 1 ) - 1 ), observaqon is consistent with the theory. But more adjustment is necessary. A.Tanaka & HN /07/ EA ALMA Development Workshop 16
17 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon CorrecQon in UV calculaqon In calculaqng UV field with Hα image, only diffuse component should be taken. Diffuse and Discrete Only Diffuse Diffuse and Discrete Only Diffuse 2013/07/ EA ALMA Development Workshop 17 A.Tanaka & HN 2012
18 1. Cosmic web 2. MagneQc field 3. Star FormaQon law 4. HI- H 2 transiqon EvoluQon of H 2 /HI EvoluQon of H 2 /HI predicted Milenium simulaqon (Springel 2005) ObservaQon of CO and HI with ALMA and SKA will be important. Study of f mol should be extended to more samples 2013/07/ EA ALMA Development Workshop 18 Obreschkow et al. 2009
19 Next ScienQfic Requirement Needs for complementary observaqon with SKA CO data with SpaQal ResoluQon: 1 Velocity ResoluQon: 10 km/s FoV: 45 SensiQvity: 10 mk Seems not so challenging (resoluqon and sensiqvity), but too large FoV. 2013/07/ EA ALMA Development Workshop 19
20 SpecificaQons In 100 hr integraqon Qme FoV: 45 x45 ResoluQon: 1 Velocity resoluqon:10 km/s Rms noise: 1 K VLA SKA ALMA Freq. 1.4GHz (HI) 1.4GHz(HI) 115GHz (CO) FoV 29 x x x45 SpaQal Res. 1.4 Velocity Res. (A- array) 10 km/s (47kHz) km/s (47kHz) 10 km/s (3.8MHz) RMS Noise 1 K 1 K 10mK *2 Required integ. Qme *1 VLA exposure calculator 29 yrs *1 6 days *1 1877days (5 yrs *3 ) (11hr*(48*60/45) 2 ) 2013/07/ EA ALMA Development Workshop 20
21 SpecificaQons In 100 hr integraqon Qme FoV: 45 x45 ResoluQon: 1 Velocity resoluqon:10 km/s Rms noise: 1 K VLA SKA ALMA Freq. 1.4GHz (HI) 1.4GHz(HI) 115GHz (CO) FoV 29 x x x45 SpaQal Res. 1.4 Velocity Res. (A- array) 10 km/s (47kHz) km/s (47kHz) 10 km/s (3.8MHz) RMS Noise 1 K 1 K 10mK *2 Required integ. Qme 29 yrs *1 6 days *1 1877days (5 yrs *3 ) (11hr*(48*60/45) 2 ) *1 VLA exposure calculator (3000 SKA antenna corresponds to 1080 VLA antenna) *2 because X CO =1.8e20 cm - 2 K - 1 km - 1 s, X HI =1.8e18 cm - 2 K - 1 km - 1 s 2013/07/09 *3 ALMA OT sensiqvity calculator 2013 EA ALMA Development Workshop 21
22 SpecificaQons In 100 hr integraqon Qme FoV: 45 x45 ResoluQon: 1 Velocity resoluqon:10 km/s Rms noise: 1 K VLA SKA ALMA Freq. 1.4GHz (HI) 1.4GHz(HI) 115GHz (CO) FoV 29 x x x45 SpaQal Res. 1.4 Velocity Res. (A- array) 10 km/s (47kHz) km/s (47kHz) 10 km/s (3.8MHz) RMS Noise 1 K 1 K 10mK *2 Required integ. Qme 29 yrs *1 6 days *1 1877days (5 yrs *3 ) (11hr*(48*60/45) 2 ) *1 VLA exposure calculator (3000 SKA antenna corresponds to 1080 VLA antenna) *2 because X CO =1.8e20 cm - 2 K - 1 km - 1 s, X HI =1.8e18 cm - 2 K - 1 km - 1 s 2013/07/09 *3 ALMA OT sensiqvity calculator 2013 EA ALMA Development Workshop 22
23 Next possible target of ALMA development 1 Increase survey speed by 300 (1877/6) Qmes if complementary observaqon with SKA is planned. too big? RealisQc goal: Increase by 30 Qmes 30- beam array OTF (cf. BEARS 25- beam) Freq. SKA ALMA 1.4GHz(HI) 115GHz (CO) FoV 48 x x45 SpaQal Res Vel. Res. 10 km/s (47kHz) 10 km/s (3.8MHz) Noise 1 K 10mK *2 Required Qme 6 days *1 1877days (5 yrs *3 ) (11hr*(48*60/45) 2 ) 2013/07/ EA ALMA Development Workshop 23
24 Next possible target of ALMA development 2 Don t forget difference of bandwidth raqo to the observed frequency Instantaneous bandwidth: - SKA: Band centre ± 50% (eg., GHz) (z<2.8 (1.4GHz)) - ALMA: Band centre ± 16% (case of Band3) (z<1.36 (115GHz)) SKA will have twice larger redshi^ coverage than the current ALMA 2013/07/ EA ALMA Development Workshop 24
25 Summary In SKA project will start a science operaqon, big changes will come in ISM study, such as (1) cosmic web, (2) magneqc field, (3) SF in low density and low metallicity environment, and (4) HI- H 2 transiqon. ALMA would need comparable survey speed with SKA Possible targets of future development for ALMA are (1) beam array, and/or (2) twice larger bandwidth. 2013/07/ EA ALMA Development Workshop 25
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