ALMA Workshop Science with Mopra for the ALMA

ALMA Workshop "Science with Mopra for the ALMA“ June 9 th 2012, NAOJ, Mitaka, Japan Survey of dense molecular gas in Southern active galaxies using Mopra Kohno Kotaro The University of Tokyo

Why I am here today • I would like to know whether it is feasible or not to use Mopra to detect a few 100 km/s width lines with a noise level of a few m. K (although I know that it is a not easy business!) • If yes, Mopra extragalactic surveys of dense molecular tracers at 3 mm band, including CN, 13 CO, CS, HCN, and HCO+, will be very important toward the understanding of the impact of AGN on the surrounding dense molecular medium.

What I want to achieve: Question: Is this feasible? (how about baseline stability? ) Typical line width: 300 -800 km/s • Typical HCN(1 -0) intensities in these CO bright galaxies (i. e. , CO(1 -0) ~ 0. 4 K in Ta* with SEST 15 m): 10 ~ 20 m. K in Ta* with SEST 15 m 1σ = 3 m. K in Ta* After smoothing down to dv=35 km/s

Outline • Importance of mm/submm spectroscopy of dense molecular medium as a new diagnostic tool of power sources in dusty galaxies • Some examples: NGC 1068 and Arp 220 • What can be seen with Mopra: some lessons from NRO 45 m spectra of nearby AGN (NGC 1068) and starburst galaxies (NGC 253 and IC 342) at 3 mm • Possible targets of Mopra extragalactic dense gas surveys and feasibility • ALMA cycle 0 observations of NGC 1097 at 0. 8 mm (350 GHz) band (if time allows)

Introduction: Importance of mm/submm spectroscopy of dense molecular medium as a new diagnostic tool of the power sources in dusty galaxies

Essential roles of dense molecular gas at the vicinity of active nuclei As a driver of activities • Feeding super massive black holes • Fueling starburst events • Obscuring the broad line regions of AGNs (obscuring torus hypothesis) As a diagnostic tool of power sources • Affected by various types of activities – AGN: hard X-ray, shock (by AGN jet) – Starburst: UV, shock (by SNe), cosmic ray

Major heating mechanisms of ISM in active galaxies • Hard X-ray: forming X-ray dominated regions (XDRs) - Maloney 1999, Ap&SS, 266, 207 • UV: forming HII regions and photo dissociation regions (PDRs) • Cosmic ray heating (mainly from SNe? ) • Mechanical heating: energy injection into the ISM by the dissipation of kinetic energy produced by shock (either AGN jet or SNe? ) – See Meijerink et al. 2011, A&A, 525, A 119 for the effects of cosmic rays and mechanical heating

Mm/submm spectroscopy as a new diagnostic probe of dusty nuclei of galaxies • The idea: To use mm/submm spectral line features as a diagnostic probe of the power source(s) of dusty nuclei of galaxies • Key questions: – What is the characteristic spectral features reflecting the effects of AGN, UV, shocks, cosmic ray, mechanical heating, etc?

Why do we need mm/submm based diagnostics? • Mm/submm lines can penetrate into the dusty nuclei of luminous galaxies – Hard X-ray: Compton thick; NIR/MIR diagnostics also have a limitation to the very dusty nuclei – Can be applied to high-z dusty quasar search? (Schleicher et al. 2010, A&A, 513, A 7) • High angular resolution can be achieved with ALMA – In the ALMA era, we will have very high angular resolution dust continuum images of galaxies (often better than HST etc. ) we have no diagnostic for two close dusty galaxies pair with a separation of <0. 1” !

How to discriminate? • HCN (Kohno et al. 2003, PASJ, 55, L 1; Krips et al. 2008, Ap. J, 677, 262; Harada et al. 2010, Ap. J, 721, 1570) • CN (e. g. , Meijerink et al. 2007, A&A, 461, 793) • Si. O (Garcia-Burillo et al. 2010, A&A, 519, A 2) • CO ladder (Rangwala et al. 2011, Ap. J, 743, 94) • H 2 O (see references in the following slides) • Vibrationally excited HCN (Sakamoto et al. 2010, Ap. J, 725, L 228) & HC 3 N (Costagliola & Aalto 2010, A&A, 515, A 71) • Measuring brightness temperature of dust continuum (Sakamoto et al. 2008, Ap. J, 684, 957; Downes & Eckart, 2007, A&A, 468, L 57)

Elevated HCN in the proto-typical Seyfert galaxy NGC 1068

NGC 1068 (AGN) • Nucleus： RHCN/CO = 0. 54 RHCN/HCO+ = 2. 1 significant enhancement of HCN • Disk (starburst ring)： RHCN/CO = 0. 10 RHCN/HCO+ = 1. 3 typical values for starburst regions Kohno et al. 2008, Ap. SS, 313, 279 Helfer & Blitz 1995 12

Millimeter-wave molecular spectroscopy as a new diagnostic of nuclear energy source AGN: CN N=1 -0 J=3/2 -1/2 • HCN/HCO+>2 -3 • CN(J=3/2 -1/2) /(J=1/2 -1/2)～ 1？ XDR chemistry? J=1/2 -1/2 Starburst: J= 1/2 -1/2 SB CN N=1 -0 J=3/2 -1/2 １ GHz幅 • HCN/HCO+＜ 1 • CN(J=3/2 -1/2) /(J=1/2 -1/2)～ 0. 3 PDR chemistry? Nobeyama Millimeter Array Kohno et al. 2008, Ap. SS, 313, 279

A diagnostic method of nuclear power source in dusty galaxies ? “Pure AGN”: Dense molecular medium affected by AGN? Nobeyama Millimeter Array NGC 1068 RHCN/HCO+ Seyfert Starburst “Composite”: AGN with a nuclear starburst ? RHCN/CO Kohno et al. 2001 (astro-ph/0206398) Kohno 2005 (astro-ph/0508420) Kohno et al. 2008, Ap. SS, 313, 279

XDR chemistry in NGC 1068 • The CND of NGC 1068 (~ 100 pc scale) is a giant X -ray Dominated Region (XDR). – Based on Si. O, CN, HCO+, HOC+, H 13 CO+ and HCO lines by IRAM 30 m Also support our view Usero et al. , 2004, A&A, 419, 897 15

変 “HCN Enhanced Nuclei” (HENs) 変 • NGC 1068 (Sy 1. 8)：Jackson et al. 1993 (NMA), Tacconi et al. 1994 (Pd. BI), Helfer & Blitz 1995 (BIMA), Kohno et al. 2008, Ap. SS, 313, 279 • NGC 5194 (Sy 2)：Kohno et al. 1996, Ap. J, 461, L 29 (NMA) • NGC 1097 (Sy 1)：Kohno et al. 2003, PASJ, 55, L 1 (NMA) • NGC 5033 (Sy 1. 5)：Kohno et al. 2005, astro-ph/0508420 (NMA) • NGC 6951 (Sy 2): Krisp et al. 2007, A&A, 468, 63 (Pd. BI) • NGC 4501 (Sy 2), NGC 4388 (Sy 2) : Kohno et al. (in prep. ; NMA)

Counter argument: Arp 220?

Arp 220, a proto-typical ultra luminous IR galaxy, also shows an elevated + HCN/HCO ratio • EMIR on IRAM 30 m telescope Still HCN/HCO+ values exceeding 2 are very rare Costagliola et al. 2011, A&A, 528, A 30 The issue: What is the power source of these ULIRGs? Arp 220 HCN/HCO+ = 2. 1 UGC 5101 HCN/HCO+ = 2. 7 +/- ? ?

Excess of HCN(1 -0)/HCO+(1 -0) in Arp 220 (and other ANG-hosting ULIRGs) Imanishi, et al. 2007, AJ, 124, 2366 Nobeyama Millimeter Array

Multi-wavelengths view of Arp 220 L(FIR) ～ 2× 1012 Lo Too dusty for hard X-ray See introduction of Martin et al. 2011, A&A, 527, 36 Av > 100 ma g !? Scoville et al. 1998, Ap. J, 492, L 107 See also Sakamoto+ For double nuclei ⇒ Numerous SNe ? Genzel & Tacconi, 1998, Nature, 395, 859 Downes & Solomon 1998, Ap. J, 507, 615

Recent big surprise provided by Herschel (and Z-Spec/CSO): 1) very high-J CO 2) water vapors

SPIRE-FTS 190 – 670 μm spectrum • df FWHM ~ 1. 44 GHz or d. V = 280 km/s – 950 km/s across the spectral range, beam size = 17” – 40” • Total on-source: 10455 sec = 2. 9 hours – Deep dark sky observations (13320 sec = 3. 7 hours) for the emission from the telescope Rangwala et al. 2011, Ap. J, 743, 94

Arp 220 SPIRE-FTS spectrum Rangwala et al. 2011, Ap. J, 743, 94 • Bright H 2 O lines & very high-J CO lines • Mechanical heating? + AGN? ~50 K ~1350 K ⇔ H 2 rotation temperatures 10% in gas mass but dominating L’co

Mkn 231 Herschel/SPIRE-FTS Van der Werf et al. 2010, A&A, 518, L 42 ~ 1200 GHz coverage !!! R ~ 400 - 1200 • Very high-J CO lines up to J=13 -12 are still well excited !!! • Very rich in species; many bright H 2 O, H 2 O+, OH+ lines

SPIRE-FTS spectrum of M 82, a pure starburst galaxy, is dominated by CO, no H 2 O Panuzzo et al. 2010

PDR vs XDR: 4 major differences • X-ray penetrate much larger column densities than UV photons • Gas heating efficiency in XDRs is very high (1050 %), compared to PDRs (< 1%) • Dust heating much more efficient in PDRs than in XDRs • High ionization levels in XDRs drive ionmolecule chemistry over large column density

Heating source modeling: XDR vs PDR • XDRs produce larger column densities of warmer gas • Identical incident energy densities give very different CO spectra • Very high-J CO lines are excellent XDR tracers • Need good coverage of CO ladder Spaans & Meijerink 2008

CO SEDs of high-z submillimeter galaxies (SMGs) • HLSW 01 is rather similar to Cloverleaf AGN powered? • Orochi: a 10^13 Lo source but likely to be powered only by starburst Inoue Hirofumi et al. , In prep.

Water vapor emission in a high-z lensed SMG Observing frequency [GHz] Pd. BI Omont et al. 2011, A&A, 530, L 3 Z-Spec/CSO Lupu et al. 2010, Ap. J, submitted (ar. Xiv: 1009. 5983) SDP. 17 b, z=2. 305 H 2 O 20, 2 -11, 1

Water vapor at z=3. 91 Bradford et al. 2011, Ap. J, 743, 167 z=3. 911 Z-Spec/CSO Van Der Werf et al. 2011, A&A, 741, L 38 ↓ Pd. BI Observing frequency [GHz] Para H 2 O 22, 0 -21, 1 Pd. BI Lis et al. 2011, Ap. J, 738, L 6

Level diagram of water lines スピン平行 スピン反平行 Van Der Werf et al. 2011, A&A, 741, L 38 ping f=1208 GHz Eu/k=454 K iati v Rad f=557 GHz Not detected Eu/k=61 K pum f=988 GHz Eu/k=101 K Radi ative f=1229 GHz Lis et al. 2011 ep um pin g f=1163 GHz Eu/k=305 K Tdust =220 K Weiss et al. 2007, A&A, 467, 955 Riechers et al. 2009, Ap. J, 690, 463 f=752 GHz Eu/k=137 K Cricital densities ~ 10^8 cm-3 !!

Water lines in APM 08279+5255 are very different from those in PDRs 21, 1 -20, 2/11, 0 -10, 1 ratio > 8 !!! Collisional excitation is unlikely. . – thermal level populations: 21, 1 -20, 2/11, 0 -10, 1 ratio is 0. 6 in Orion bright bar (PDR): White et al. 2010, A&A, 518, L 114; Habart et al. 2010, A&A, 518, L 116 Populated by the absorption of FIR photons Excited by collision – much fainter than CO lines in the same freq. range: H 2 O 21, 1 -20, 2 /CO(6 -5) luminosity ratio is 0. 026 in Orion bar ⇔ 0. 6 ! in APM 08279 Radiative pumping Unimportant as a coolant of warm dense gas?

Interim summary • Mm/submm spectra contain rich information on the impact of the power sources onto the surrounding dense interstellar medium. • Although we need further studies (with ALMA) on the spatially resolved physical and chemical properties of dense ISM in both AGN and starburst galaxies, 3 mm lines such as HCN can be a diagnostic probe of AGN.

What can be seen with Mopra: Key features at 3 mm band Some lessons from unbiased spectral line scans at 3 mm using NRO 45 m telescope (and supporting evidence by ALMA cycle 0 data!) toward nearby AGN and starbursts

Unbiased line surveys with NRO 45 m SAM 45+PANDA+T 100/TZ 100 on NRO 45 m telescope 30 GHz coverage, 0. 5 HCN(1 -0)/CS(2 -1) MHz resolution @100 GHz R~2 x 105, dv~1. 5 km/s > 5 @NGC 1068 32 GHz coverage (AGN) sub-m. K sensitivity Nakajima, Takano, Kohno et al. 2011, Ap. J, 728, L 38; in prep. HCN(1 -0)/CS(2 -1) < 2 @NGC 253, IC 342 (starburst) 85 90 95 Frequency [GHz] 110 115

Unbiased line surveys with NRO 45 m SAM 45+PANDA+T 100/TZ 100 on NRO 45 m telescope 30 GHz coverage, 0. 5 MHz resolution @100 GHz R~2 x 105, dv~1. 5 km/s CN(N=1 -0)>13 CO(1 -0) @NGC 1068 (AGN) 32 GHz coverage sub-m. K sensitivity Nakajima, Takano, Kohno et al. 2011, Ap. J, 728, L 38; in prep. CN(N=1 -0)<13 CO(1 -0) @NGC 253, IC 342 (starburst) 85 90 95 Frequency [GHz] 110 115

Then, why not use Mopra!

Importance of Mopra • Measuring the intensities of major dense gas tracers at 3 mm toward CO bright southern galaxies – Many (possibly) CO bright southern galaxies remain unexplored yet! • Key lines are: CN(N=1 -0), 13 CO(J=1 -0), CS(J=2 -1), HCO+(J=1 -0), HCN(J=1 -0) – Mopra measures ground state lines, whereas ASTE observes higher order lines multi N/J measurements are essential to quantify the abundance and excitation separately. – Single dish measurements an indispensable step toward ALMA proposals (high resolution imaging)

Southern (<-35 deg) gas rich (>0. 1 K in SEST) active spiral galaxies in Ta* scale Name Decl. Activity CO(1 -0) brigthness (SEST 15 m, Ta*) NGC 4945 -49 deg Sy 2+SB 1. 3 K Curran et al. 2001, A&A, 367, 457 NGC 986 -39 deg SB 0. 4 K Elfag et al. 1996, A&A Suppl. 115, 439; see also CO(3 -2) ASTE, Kohno et al. 2008, PASJ, 60, 457 Circinus -65 deg Sy 2+SB? 0. 4 K Curran et al. 2001, A&A, 367, 457 NGC 1365 -36 deg Sy 1. 8 0. 4 K Elfag et al. 1996, A&A Suppl. 115, 439 NGC 3256 -43 deg SB? 0. 3 K Casoli et al. 1992, A&A, 264, 49 NGC 7552 -42 deg Sy 2+SB 0. 2 K Claussen & Sahai 1992, AJ, 103, 1134 (also CO(3 -2) ASTE, HCN(1 -0) etc w/ ATCA) NGC 1808 -37 deg Sy 2 0. 2 K Aalto et al. 1994, A&A, 286, 365 NGC 7130 -35 deg SB? 0. 17 K Elfag et al. 1996, A&A Suppl. 115, 439 NGC 1672 -59 deg AGN+SB? 0. 13 K Bajaja et al. 1995, A&A Suppl. 114, 147 (also CO(3 -2) ASTE) NGC 7582 -42 deg Sy 1+SB? 0. 13 K Claussen & Sahai 1992, AJ, 103, 1134 NGC 3620 -76 deg SB? 0. 12 K Elfag et al. 1996, A&A Suppl. 115, 439 NGC 2369 -62 deg SB? 0. 12 K Elfag et al. 1996, A&A Suppl. 115, 439

ASTE CO(3 -2) observations of some Southern spirals have been started • Discovery of “dense gas rich bar” in NGC 986 dynamically young bar? Kohno et al. , 2008, PASJ, 60, 457

What I want to achieve: Question: Is this feasible? (how about baseline stability? ) Typical line width: 300 -800 km/s • Typical HCN(1 -0) intensities in these CO bright galaxies (i. e. , CO(1 -0) ~ 0. 4 K in Ta* with SEST 15 m): 10 ~ 20 m. K in Ta* with SEST 15 m 1σ = 3 m. K in Ta* After smoothing down to dv=35 km/s

Summary • Importance of mm/submm spectroscopy of dense molecular medium as a new diagnostic tool of power sources in dusty galaxies • Some examples: NGC 1068 and Arp 220 • What can be seen with Mopra: some lessons from NRO 45 m spectra of nearby AGN (NGC 1068) and starburst galaxies (NGC 253 and IC 342) at 3 mm • Possible targets of Mopra extragalactic dense gas surveys and feasibility • ALMA cycle 0 observations of NGC 1097 at 0. 8 mm (350 GHz) band (if time allows)

ALMA cycle 0 band 7 data of the southern AGN+SB hybrid galaxy NGC 1097 PI. =K. Kohno, ID=2011. 0. 00108 S Special thanks to Daniel Espada

Active nucleus of NGC 1097 • CO(2 -1)/CO(1 -0) =1. 8 ± 0. 2 • Presence of strong heating source(s) is suggested ! In Tb scale CO(1 -0) NMA CO(2 -1) SMA 1 kpc VLT MELIPAL + VIMOS 1 kpc Hsieh et al. , 2008, Ap. J, 683, 70 Kohno et al. 2003 PASJ, 55, L 1

ALMA cycle 0 band 7 observations • Two observing runs @Compact configuration – 5 th Nov. 2011, UT 06: 51 -07: 54, 14 ant, (on~28 min. ) – 6 th Nov. 2011, UT 02: 05 -03: 09, 15 ant, (on~28 min. ) • Calibrators – Bandpass: J 0522 -364, visibility : J 0334 -401 + Callisto • Achieved noise level – ~2. 1 m. Jy@LSB, ~2. 3 m. Jy @USB @df=9. 766 MHz • cf. on-source 1. 1 hrs is required according to OT mostly consistent with the OT’s expectations ! • This noise level is compatible to that in typical one night SMA continuum imaging for SMGs (~2 m. Jy rms) !!!

Flux density [m. Jy/beam] LSB spectrum (SPW 0/SPW 1) higher frequency part (i. e. , blue shifted) of the emission Is chopped CS(7 -6) HC 15 N(4 -3) H 13 CN(4 -3) Before CLEAN Observed Frequency [GHz]

Close up view of SPW 0 Flux density [m. Jy] No CS(7 -6) emission !! f_rest = 342. 883 GHz f_obs = 341. 449 GHz HC 15 N(4 -3) < 4. 2 m. Jy (2σ upper limit) Superb ALMA sensitivity imposes a significant, meaningful upper limit if we compare the CS(7 -6) with HCN(4 -3). Observing frequency [GHz] f_obs ~ 342. 75 GHz 1σ ~2. 1 m. Jy for dv=8 km/s !!!

Flux density [m. Jy/beam] USB spectrum (SPW 2/SPW 3) HCN(4 -3) HCN(v 2=1, l=1 f, J=4 -3) f_rest = 356. 256 GHz, f_obs = 354. 766 GHz HCO+(4 -3) ? ! Observed Frequency [GHz] 1σ ~2. 3 m. Jy

Close of views of HCN and HCO+ J=4 -3 Flux density [m. Jy/beam] Very good S/N as if they were CO !!! Incredible !!! Observing frequency [GHz]

Striking difference of B 7 spectra between NGC 1097 and NGC 4418 Sakamoto et al. 2010, Ap. J, 725, L 228 NGC 4418 spectra CS(7 -6) ~ 66 m. Jy Significant radiative excitation of HCN(4 -3) ~ 133 m. Jy HCN(v 2=1) ~ 30 m. Jy HCN(4 -3)/CS(7 -6) ~ 2. 0 @4418, > 10 @1097 HCO+(4 -3) ~ 82 m. Jy Weakness of CS w. r. t. HCN is evident in NGC 1097 enhancement of HCN? !

Comparison of B 7 line peak fluxes HCN(4 -3) NGC 1097 [m. Jy] 40 NGC 4418 [m. Jy] 133 Ori-KL [K] in Tmb 50 R-Cr. A [K] in Tmb 4. 3 HCO+(4 -3) 23 82 47 19. 6 HCN(v 2=1, J=4 -3) CS(7 -6) <4. 6 30 7 <0. 06 <4. 2 63 29 5 CO(3 -2) ~900 746 145 35 Schilke+, 1997, Ap. JS, 108, 301 Watanabe+ 2012 Ap. J, 745, 126 This work HCN(v 2=1, 4 -3)/ HCN(4 -3) <0. 12 Sakamoto+ 2010, Ap. J, 725, L 228 0. 23 0. 14 <0. 014 HCN(4 -3)/CS(7 -6) > 10 2. 0 1. 7 NGC 4418 is very similar to massive. SF regions, whereas the nucleus of NGC 1097 is different from them 0. 86