wsma for Nearby Galaxies

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1 wsma for Nearby Galaxies Kazushi Sakamoto (ASIAA) The overview talks should focus future discussion on what the upgrade will better enable in their particular area of expertise, rather than summarizing what has been done to date. SOC Ideas for exciting science with wsma on nearby galaxies?

2 wsma in the ALMA era Northern Sky, Nearby targets δ(alma) < +47. Ω(no ALMA)= 0.54 π str = 13% of sky SMA ALMA for same linear resolution and T b sensitivity when SMA targets are 5 times closer High Site/Submm (compared to NOEMA) Wide Bandwidth (28 GHz compared to ~7GHz with ALMA) Wide FOV for el. > 20 or 20 % for el.(alma) < 30 Intermediate Resolution (~3 ) Path Finder (quick turnaround, easy access) Time Domain (UT coverage, high cadence) afternoon session

3 Northern Nearby Galaxies No ALMA δ(alma) < +47. Ω(no ALMA)= 0.54 π str = 13% of sky for el. > 20 or 20 % for el.(alma) < 30 name Dec.[ ] D [Mpc] note M nearest/protorype starburst M LLAGN, variable IC face-on spiral, starburst Maffei starburst NGC face-on spiral, starburst Arp merger, L IR = L Mrk nearest quasar (L IR = L ) Mrk ULIRG (L IR = L ) M face-on spiral M face-on spiral, LLAGN NGC Seyfert NGC C84, AGN(Sy) M Andromeda galaxy NGC Seyfert (binary BH?) Other LIRGs UGC5101, VII Zw 031, NGC6090, NGC4194, next talk

4 Northern Nearby Galaxies (face-on) spirals : M31, M81, IC342, NGC6946, M101, M51 molecular cloud properties, SF-law, spiral arm/density wave Starbursts : M82, IC342, Maffei 2, NGC6946, elevated SF (SF-law, m.c. properties in SB), evolution (trigger, feedback, quenching) Merger/U,LIRG: Mrk 231, Mrk273, Arp 299 (NGC3690+IC694) extreme SF (SF-law, mol. gas properties in extreme SB), evolution(trigger, feedback), Eddington-limit SF AGN : Mrk 231, NGC1275 (3C84), 3516, 4051, 4151; M81, M51 feeding/feedback, effects of AGN (X-ray, jet) on ISM, AGN time variability

5 Northern Nearby Spirals M31, M81, NGC6946, hysical Journal, 779:42 IC342, (29pp), 2013 December 10M101, 4 1 (40pc) in CO(1-0) M51 (<10Mpc) (Schinnerer+ 13)

6 Northern Nearby Spirals M31, M81, NGC6946, hysical Journal, 779:42 IC342, (29pp), 2013 December 10M101, M51 (<10Mpc) - fraction of CO in GMCs - MC size, Lco, Tb, M fn. - σ, α - scaling relations - ICO PDF - SF law - GMC lifetime - local variation of these 4 1 (40pc) in CO(1-0) (Schinnerer+ 13)

7 Northern Nearby Spirals M31, M81, IC342, NGC6946, M101, M51 (<10Mpc) M51 5 Spitzer/SINGS,LVL

8 Northern Nearby Spirals M31, M81, IC342, NGC6946, M101, M51 (<10Mpc) CO(1-0) 2 (85pc) Nieten+ 06 IRAM 30m M51 possible VERY-LARGE project

9 Technical Wish List Fantastic to have multi-pixel receivers Nice to have IF=4-20 GHz for stacking analysis of non- 12 CO lines RF=[230,246]+[254,270] RF=[330,346]+[354,370] 13 HCO + HCN(4-3) HCO + @362.6

10 Starburst-Prototype : M82 M82 Chandra 1064 KETO, HO, & LO Vol. 635 SMA Keto et al (17pc)

Southern Starburst-Prototype : NGC 253 The Astrophysical Journal, 801:63(19pp),2015March1 Meier et al. HCN HCO + Meier et al. 2015 ALMA Cyc.

13 CO + HN 13 C Dec. Offset (") Dec. Offset (") 30 20 10 0 10 20 30 30 20 10 0 10 20 30 500 400 300 200 100 1.4 1.2 1 0.8 0.6 0.4 0.2 0 9 10 86 86.5 87 87.5 88 88.5 89 CO C 17 O 7 Figure 2.

11 Southern Starburst-Prototype : NGC 253 The Astrophysical Journal, 801:63(19pp),2015March1 Meier et al. HCN HCO + Meier et al ALMA Cyc. 0 Extended Compact CN CN CO C 2 H complex CS HC 3 N S ν (mjy beam 1 ) H 13 CN SiO SO CH C H 3 2 H 2 CS CH 3 SH NH CHO 2 H CS 2 C 2 S C 17 O CO (v=1)/c 4 H NS NS 10 2 SO HNCO H52β H40α HCOOH HC 15 N H 13 CO + HN 13 C Dec. Offset (") Dec. Offset (") CO C 17 O 7 Figure 2. Extracted spectrum near the center of NGC 253 (position 5 inc Figure 2 H 4), on a logarithmic scale. To deal with subtle issues regarding the bandpass calibration, GHz GHz the data have been 1.5 independently continuum subtracted 6 for each spectral GHz window. After that, the average continuum flux density in a given spectral window was total molecular gas τ<1 molecular gas added to the spectrum. The flux density offset between the observations PDR obtained in the compact and extended configurations is real; the observations in thecompact 5 configuration recover more of the extended flux. As in Figure 1, identifiedmolecularspectrallinesarelabeled(secure:bold,tentative:italics,seetable1 for full 1 4 description of transitions) Integrated line maps. We created line 2 cubes for each line, and then blanked those with a mask derived from the CO(1 0) 1 0 line (by far the brightest line in the bandpass). 0 The integrated intensity map for a given line was then derived by simply adding all data in the respective data cube (without any further flux 2 H40α 14 HNCO cutoff). Integrated line maps are corrected for primary beam attenuation and are shown in Figure HCN GHz GHz GHz 12 RRL dense gas 1.5 weak shocks 10 Uncertainties. We calculated error maps by taking the number of channels per pixel into account. An inspection of the data cubes 2 revealed 6 that these error maps provide too optimistic uncertainties, as they do not account for artifacts (in particular 3 the negative 2 bowl due to the missing short spacings) in the current data. 0 We thus adopt a conservative 0 10% error for Frequency (GHz) It is not possible to estimate the percentage of detected flux for every line in the survey because suitable single-dish observations are often not available. We do, however, determine this fraction for a number of transitions where possible. For the following transitions we calculate detected flux percentages over single-dish beam of of: HCN(1 0) 100% (Paglione et al. 1995), HCO + (1 0) 55% (Martín et al. 2009b), C 17 O(1 0) 60% (Henkel et al. 2014), SiO(2 1) 110% (Martín et al. 2009b), CN(1 0;(3/2) (1/2)) 60% (Henkel et al. 2014), C 2 H(1 0;(3/2) (1/2)) 60% (Nakajima et al. 2011), and HNCO( ) 50% (Nguyen-Q-Rieu et al. 1991; though this value is highly uncertain because HNCO does not peak where Nguyen-Q-Rieu et al. pointed). Therefore, it appears

12 slide from S. Martin Not all starbursts are the same M82 chemistry with SMA Poster N. Harada

13 Spatially-resolved Wide-band Spectroscopy on Starbursts 1.0 PWV= 0.25 mm; 5% of ALMA time PWV= 1 mm; 50% of ALMA time 0.8 Transmission Band 3 Band 4 Band 5 Band 6 wsma Band 7 Band O2@119 H2O@183 H2O@325 H2O@380 O2@368 O2@425 H2O@448 H2O@475 O2@ Frequency / GHz full scan or selected lines? Frequency / GHz

14 Path Finder (for ALMA) Flux Density [Jy] First extragalactic detection of rotational lines from vibrationally-excited HCN HC 3 Nv 7 F (rest) [GHz] HCN(3 2) HCNv 2 HCO + (HCN) C273 x 0.07 (HCO + ) ±1σ (by IR radiation) Flux Density [Jy] HCN(4 3) HC 3 N(39 38) F (rest) [GHz] HC 3 Nv 7 HCN(v 2 =1) HCO + (4 3) 3C273 x 0.1 (HCN) (HCO + ) ±1σ Energy / k [K] v 2 =1 v=0 J=4 H C N J=3 J=2 J=1 J=4 H C N J=3 J= F (obs.) [GHz] F (obs.) [GHz] Sakamoto+2010, SMA filler program 0 J=1 J=0 ~10 ALMA projects have been approved for HCN-vib. Also, SMA very useful to justify higher-res. ALMA obs.

15 Intermediate Resolution Table A-1: Angular Resolutions (AR) and Maximum Recoverable Scales (MRS) for the Cycle 4 Array configurations Config Lmax Band Band 3 Band 4 Band 6 Band 7 Band 8 Band 9 Band 10 Lmin Freq 100 GHz 150 GHz 230 GHz 345 GHz 460 GHz 650 GHz 870 GHz 7-m m AR 12.5" 3.7" 2.5" 8.4" 1.6" 5.4" 1.1" 3.6" 0.80" 2.7" 0.57" 1.9" 0.42" 1.4" C40-1 Array 159 m MRS 29.0" 66.7" 19.4" 44.5" 12.6" 29.0" 19.3" 8.4" 14.5" 6.3" 10.3" 4.5" 3.3" 7.7" C40-2 C m AR 2.4" 3.7" 1.6" 2.5" 1.0" 1.6" 0.69" 1.1" 0.52" 0.80" 0.37" 0.57" 0.27" 0.42" At GHz C40-2 lowest resolution of ALMA main array ~ single-dish beam 5 C40-4 C40-3 whereas SMA beam ~ (COM@250, SUB@350) C40-5 C40-4 C40-6 C40-5 C40-7 C m MRS 29.0" 19.4" 12.6" 8.4" 6.3" 4.5" 3.3" 273 m AR 2.4" 1.6" 1.0" 0.69" 0.52" 0.37" 0.27" 15 m MRS 22.1" 14.8" 9.6" 4.0" 6.4" 3.0" 4.8" 2.1" 3.4" 1.6" 2.5" m AR 0.93" 1.5" 0.62" 0.97" 0.40" 0.63" 0.27" 0.42" 0.20" 0.32" 0.14" 0.22" 0.11" 0.17" 15 m MRS 13.7" 8.9" 5.9" 9.1" 3.9" 5.9" 2.6" 4.0" 1.9" 3.0" 1.4" 2.1" 1.0" 1.6" km AR 0.54" 0.93" 0.36" 0.62" 0.23" 0.40" 0.16" 0.27" 0.12" 0.20" 0.083" 0.14" 0.062" 0.11" m MRS 6.0" 8.9" 4.0" 5.9" 2.6" 3.9" 1.7" 2.6" 1.3" 1.9" 0.93" 1.4" 0.69" 1.0" km AR 0.35" 0.54" 0.23" 0.36" 0.15" 0.23" 0.10" 0.16" 0.076" 0.12" 0.054" 0.083" 0.040" 0.062" any unique science at ~3? m MRS 3.1" 6.0" 2.1" 4.0" 1.3" 2.6" 0.90" 1.7" 0.67" 1.3" 0.48" 0.93" 0.36" 0.69" km AR 0.21" 0.35" 0.14" 0.23" 0.090" 0.15" 0.060" 0.10" 0.045" 0.076" 0.032" 0.054" 0.024" 0.040" m MRS 1.8" 3.1" 1.2" 2.1" 0.77" 1.3" 0.52" 0.90" 0.39" 0.67" 0.27" 0.48" 0.20" 0.36"

16 Some Suggestions Requests for the upgrade Minimize Tsys. Maximize stability & efficiency (8-ant op.) Dual-freq. not needed, multi-pix great (but too risky?) seeing-correction WVR? Programs Large/legacy projects (e.g., for N-targets) Flexible, pilot/exploratory projects (leading ALMA) Data Reduction CASA (data translator) MIR/MIRIAD an obstacle to new users Coordination with other facilities GLT, JCMT, LMT, NOEMA, etc.

17 wsma for Nearby Galaxies Summary ~15% of the sky is w/o ALMA. It has nearest L * galaxy (M31), nearest starburst (M82), nearest quasar (Mrk 231) as well as many local face-on spirals (M81, M101, IC342, ), starbursts and Seyferts. Legacy projects for these N sources e.g. large-area mapping, spectral scans Path finder to lead ALMA projects New ideas (~3 res. targets, time-domain, )

The Unbearable Lightness of Chemistry

Z H IG C G N I OM H T A P U The Unbearable Lightness of Chemistry The Unbearable Lightness of Chemistry ~ 0.5 % Molecular (H 2 ) ~ 0.002 % CO ~ 0.000002 % any other molecule A total of 46 molecular species