In the era of ALMA

Loretta Gregorini

Universita’ di Bologna

IRA-INAF

•Up to 64x12m Up to 64x12m Antennas Antennas

•Frequency range 30-Frequency range 30-1000 GHz (0.3-10mm)1000 GHz (0.3-10mm)

•High resolution and High resolution and sensitivitysensitivity

•Mid 2006: European ARC activities begin •Late 2007: First antennas arrive in Chile •Late 2008: Two antenna interferometry •Early 2009: Commissioning and science verification starts •2010/2011: Early science (16 ants + 4 rec. bands)•Late 2013: Full science operations starts

ALMA timeline

All atmospheric windows between 30 and 950 GHz

Initial priority to band

3= 84 to 116 GHz,

4= 125 to 169 GHz,

6= 211 to 275 GHz,

7= 275 to 373 GHz,

8= 385 to 500 GHz,

9= 602 to 720 GHz

<0.1 pwv measured with APEX

ALMA Science Requirements

•High fidelity imaging

•Precise imaging at 0.1 arcsec resolution

•Routine sub-mJy continuum sensitivity

•Routine mK spectral sensitivity

•Wideband frequency coverage

•Wide field imaging mosaicing

•Submillimeter receiver capability

•Full polarization capability

•System flexibility

1.The ability to provide high-quality and high resolution imaging in the millimeter and submillimeter bands to match that of HST and ground-based AO-equipped telescopes

2.Detecting CO and [C II] in a Milky Way galaxy at z=3 in less than 24 hours of observation

3.To map dust emission and gas kinematics in protoplanetary disks

Blue, Seyferts

Red, LINERs

Green, Transition objects

Stars, Sy+L+Tran

Magenta, HII nuclei

Ho 2008

Fueling the AGN: LLAGNs in nearby galaxies

Active nuclei in 50-70% for Hubble types E-Sb:

LINERs are the most populous constituents (2/3 of AGN)

Spectra for 486 galaxies with BT > 12

NUGA: The Seyfert 2 galaxy NGC 3147 (Casasola et al., 2008)

CO(1-0)

(“)

(“

)

1”=180pc

-

nuclear peak (AGN position) + 2 molecular rings or pseudo-rings (at r~1.8 kpc and r~3.6 kpc) in C0(1-0), which consist of individual GMC complexes with mass of a few 107 - 108 M.

M(H2) = 3.8 x 109M (in agreement with Young et al 95)

Only the internal ring M(H2) = 2 x 109M

PdBI+30m

Beam=1.8’’x1.6’’

~1.8

kp

c

~3.6

kp

c

NGC 2782 (Hunt et al. 2008)

NGC 6574 (Lindt-Krieg et al. 2008)

Results of the model and gas fueling in NGC3147Casasola et al., 2008

The bar is contained inside the first CO ring.

near-infrared J image + CO(1-0)

The authors concluded that molecular gas is presently inflowing to the center (feeding rate ~0.5 M⊙/yr), and probably feeding the low-luminosity Seyfert 2 observed in NGC 3147.

How to remove the angular momentum of the gas and to bring it to the centre to feed the AGN

Imaging molecular materal in the vicinity of AGNs Map the CO (2-1) line emission in 2 nearby AGN

(NGC1068, NGC1097)

•Band 6 (220 GHz)

• With a resolution of ~0.06 arcsec (corresponding to 5pc at 17Mpc distance)

• Sensitivity sufficient to detect T >20K gas close to AGN with ~S/N ~10

• Total integration time ~64h

ALMA ALMA

Nuclear Dense Gas in AGN Map the HCN line emission in 6 nearby AGN-Starburst Galaxies to identify the exitation source

(NGC1068, NGC2273, Arp220…)

•Band 6 (265 GHz)

• With a resolution of ~0.1 arcsec

• Total integration time ~96h

ALMA ALMA

Molecular gas in elliptical radio galaxies (The 3C/B2 sample)

52 3CR/B2 radio galaxies

28 detected in CO(1-0) and/or CO(1-2)

M(mol) ~4x108 Msol (similar to Seyfert)

T(dust)~35.4 K (IRAS)

Flaquer et al. 2008

IRAM-30m

No dust in galaxy core

no CO detection

CO line detection dust in inner galaxy core [<5-10 kpc]

HST HST

0120+33

HST

1217+291321+31

Molecular gas in elliptical radio galaxies (The B2 sample)

Prandoni et al. in preparation

Double-horn CO lines associated to rotating dusty disks

HST

Mount Wilson

0149+35

1122+39

Prandoni et al. in preparation

High-z CO AGN (Omont 2008)

In the list of Solomon & Vanden Bout

(2005):

14 SMGs with z=1.06-3.41

16 QSO with z=1.42-6.45

5 Radio Galaxies with z=2.39-5.20

All the 11 objects with z>3.5 are prominent AGN:

•H2 masses ~1010 Msol

•CO linewidths ~200-800 km/s (QSO lower end, RG upper end)

•High fraction of interacting objects

ALMAALMAImaging CO in QSO at z=4 to 6.4

To determine the the dynamical mass of the host galaxy and to provide information on the nature and physical conditions of the earliest galaxies

•Band 3 (100 GHz) (transition 4-5 redshifted)

•Resolution about 0.2 arcsec

•Brightness ~0.1 mJy/beam for a 50 km/s channel

•~ 12-20h of integration per source

The grey-scale represents the noise level, which is at the positions of the extracted sources in the range from 0.3 to 4.3 mJy/beam . The circles indicate the positions of the secure sample of 34 counterparts extracted from the sub-mm map.

SURVEY: GOODS-N with SCUBA

by Borys et al. 2003; Blake et al. 2006

850micron

10x16.5 arcmin

~480 h

~ 30 sources

Ability to provide high-quality and Ability to provide high-quality and

high resolution imaginghigh resolution imaging

With ALMA

Band 6/7 280GHz

~ (1500 pointings) 900 h

~ 0.1 arcsec resolution

~ noise 0.02 mJy

~ 3000 sources

The goal of the ALMA Design Reference Science Plan (DRSP) is to provide a prototype suite of high-priority ALMA projects that could be carried out in ~3-4 years of full ALMA operations. The DRSP serves as a quantitative reference for developing the science operations plan, for performing imaging simulations, for software design, and for other applications within the ALMA project.

•DRSP 2.0: Extension to ALMA bands 4, 5, and 8, and ACA. DRSP2 will become generally available in July, after all project reviews have been processed. www.strw.leidenuniv.nl/~alma/drsp.shmtl

EU Projectscientist

ESO DG

Head ofData Management

Operations

EU ARCManager

User Science Support

Archive Operations

ESO+Regional nodes

Bonn-Bochum-Cologne (D)

IRAM (Grenoble; F, E)

IRA, Bologna (I)

Leiden (NL)

Nordic (Onsala; DK, S, SU)

Manchester (UK)

Lisbon (P); Zürich (CH); Prague (CZ)

ARC - EUROPEARC - EUROPE

Corefunctions

ALMA DivisionHead

www/ira.inaf.it/inaf_ira/ARC-ALMA.html

ALMA Regional Centre at ESO

User support services:

•Proposal calls•Evaluation•Observation preparation•Basic data analysis support •ALMA Archive operations

Coordinating the ARC network to ensure that it is effective in supporting all parts of the ESO community, in particular ESO will ensure that software development and distribution within the European ARC is efficient.

Areas of expertise in EU ARC-nodesAreas of expertise in EU ARC-nodes1. Wide-field, high-dynamic range imaging (UK/NL/F)2. Mosaicing (I) 3. High-frequency observing (NL)4. Infrastructure for advances data analysis tools (D/NL/Nordic)5. Data handling/GRID-technology (I/P) 6. Coordinating surveys/key projects (I)7. Polarimetry (I/F/D)8. Astrometry (Nordic/D/UK)9. Pipeline heuristics (D)10. Automatic data calibration (D)11. Data pipelining (UK)12. Multi-frequency synthesis (Nordic/UK)13. Array combination imaging (UK)14. Robust self-cal methods and use of WVR data (Nordic)15. Data handling and server (P)16. Instrumental calibration (F)17. Atmospheric phase calibration (F)18. ALMA imaging simulations (F)

www/ira.inaf.it/inaf_ira/ARC-ALMA.html