The Local Volume H I Survey

ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez

The Local Volume H I Survey The Local Volume H I Survey

Ángel R. López-SánchezÁngel R. López-SánchezBärbel S. Koribalski & the LVHIS teamBärbel S. Koribalski & the LVHIS team

Ángel R. López-SánchezÁngel R. López-SánchezBärbel S. Koribalski & the LVHIS teamBärbel S. Koribalski & the LVHIS team

CSIRO /Australia Telescope National Facility (ATNF, Australia) Gas and Stars in Galaxies: A Multi-Wavelength 3D PerspectiveGas and Stars in Galaxies: A Multi-Wavelength 3D Perspective

ESO Workshop – Garching – 10 Jun 2008ESO Workshop – Garching – 10 Jun 2008

CSIRO /Australia Telescope National Facility (ATNF, Australia) Gas and Stars in Galaxies: A Multi-Wavelength 3D PerspectiveGas and Stars in Galaxies: A Multi-Wavelength 3D Perspective

ESO Workshop – Garching – 10 Jun 2008ESO Workshop – Garching – 10 Jun 2008


Galaxies in the Local VolumeGalaxies in the Local Volume Local Volume: 10 Mpc (vLG< 550 km/s) ~ +500 galaxies Region in which accurate distances are obtained. It permits multiwavelengths analysis, in particular H I surveys.

Local Volume: 10 Mpc (vLG< 550 km/s) ~ +500 galaxies Region in which accurate distances are obtained. It permits multiwavelengths analysis, in particular H I surveys.

From Karachentsev et al. 2004 (based on 450 LV galaxies with D < 10 Mpc)

M83M83 and and CenACenA groupingsgroupings

M81M81 and and IC342IC342 groupingsgroupings

SculptorSculptor groupgroup


Galaxies in the Local VolumeGalaxies in the Local Volume Local Volume: 10 Mpc (vLG< 550 km/s) ~ +500 galaxies Region in which accurate distances are obtained. It permits multiwavelengths analysis, in particular H I surveys.

Local Volume: 10 Mpc (vLG< 550 km/s) ~ +500 galaxies Region in which accurate distances are obtained. It permits multiwavelengths analysis, in particular H I surveys.

From Karachentsev et al. 2004 (based on 450 LV galaxies with D < 10 Mpc)

HIPASS

LVHIS

HIPASS: H I Parkes All Sky Survey HIPASS: H I Parkes All Sky Survey LVHIS: +70 galaxies from the ATCA LVHIS: +70 galaxies from the ATCA


LVHIS observationsLVHIS observations

Deep H I line & 20 cm radio continuum observations for all nearby (vLG< 550 km/s, D < 10 Mpc) gas-rich galaxies (HIPASS) with δ < -30º

– Full 12h x 3 ATCA arrays (EW367, 750m, 1.5km) Angular resolution of 40” – 200” (1 – 5 kpc at D = 5 Mpc)

Velocity resolution of 4 km/s

HI column density 5 x 1019 cm-2 (for 60” beam)

– Expand to GMRT, VLA, WSRT

Deep H I line & 20 cm radio continuum observations for all nearby (vLG< 550 km/s, D < 10 Mpc) gas-rich galaxies (HIPASS) with δ < -30º

– Full 12h x 3 ATCA arrays (EW367, 750m, 1.5km) Angular resolution of 40” – 200” (1 – 5 kpc at D = 5 Mpc)

Velocity resolution of 4 km/s

HI column density 5 x 1019 cm-2 (for 60” beam)

– Expand to GMRT, VLA, WSRT

LVHIS team

Bärbel Koribalski (ATNF, PI)Ángel R. Lopez-Sanchez (ATNF)

Lister Staveley-Smith (UWA)Jürgen Ott (NRAO)

Erwin de Blok (U. Capetown)Helmut Jerjen (ANU)

Igor Karachentsev (SAO, Russia)Janine van Eymeren (U. Bochum / ATNF)

Emma Kirby (ANU / ATNF)Nic Bonne (ANU / ATNF)

LVHIS team

Bärbel Koribalski (ATNF, PI)Ángel R. Lopez-Sanchez (ATNF)

Lister Staveley-Smith (UWA)Jürgen Ott (NRAO)

Erwin de Blok (U. Capetown)Helmut Jerjen (ANU)

Igor Karachentsev (SAO, Russia)Janine van Eymeren (U. Bochum / ATNF)

Emma Kirby (ANU / ATNF)Nic Bonne (ANU / ATNF)

http://www.atnf.csiro.au/research/LVHIS

COMPLETE NOW! COMPLETE NOW!


LVHIS objectivesLVHIS objectives

Deep H I imaging of all nearby, gas-rich galaxies

– Integrated HI distribution galaxy diameters, asymmetries, tidal tails, companions

– Mean HI velocity field Vrot (r), incl (r), PA (r)

– Mean HI velocity dispersion multiple components, line broadening

Deep 20-cm radio continuum imaging– Star formation rates

Globally and locally Deep H-band and Hα imaging,

and multiwavelength comparison (UV, Opt, NIR, FIR)

Deep H I imaging of all nearby, gas-rich galaxies

– Integrated HI distribution galaxy diameters, asymmetries, tidal tails, companions

– Mean HI velocity field Vrot (r), incl (r), PA (r)

– Mean HI velocity dispersion multiple components, line broadening

Deep 20-cm radio continuum imaging– Star formation rates

Globally and locally Deep H-band and Hα imaging,

and multiwavelength comparison (UV, Opt, NIR, FIR)

ESO 154–G023

ESO 215–G009

NGC 7793

NGC 1313 + AM0319–662

NGC 253

NGC 5253

NGC 5253 20cm cont + R image

IC 5052 H I map (blue) + H (green) + H

(red) (Kirby et al. 2008)

NGC 5253 20cm cont + R image

IC 5052 H I map (blue) + H (green) + H

(red) (Kirby et al. 2008)


HI and total mass distribution in the Local Volume

HI mass function & optical luminosity function

HI vs optical diameter

MHI/LB , MHI/LH ratios

Detailed rotation curves Dark Matter distribution

(Baryonic) Tully-Fisher relation

Local galaxy environments (tidal features, etc.)

Galaxy spin vector alignments

Star formation rates

The local Hubble flow and dispersion

…

HI and total mass distribution in the Local Volume

HI mass function & optical luminosity function

HI vs optical diameter

MHI/LB , MHI/LH ratios

Detailed rotation curves Dark Matter distribution

(Baryonic) Tully-Fisher relation

Local galaxy environments (tidal features, etc.)

Galaxy spin vector alignments

Star formation rates

The local Hubble flow and dispersion

…

LVHIS ScienceLVHIS Science

M 83 (NGC 5236)

Late type spiral galaxy in the Cen A Group.

Type: – SAB(s)c, – H II starburst;

Optical diameter – 12.9' x 11.5',

Dcepheid – 4.5 ± 0.3 Mpc.

UGCA 365

Visible (8.2m VLT) H I map

ATCA mosaic, Koribalski et al, in p.

– MHI = 8 109 M

– HI extend > 80 kpc– Streamers,– Asymmetric

tidal arm, – Diffuse emission, – H I distribution is

ENORMOUS, several times larger than its stellar disk

H I velocity field:– Thoroughly twisted velocity field– Mildly interacting with the neighbouring dwarf galaxies– It seems to be a distorted one-armed spiral, suggesting that it may have interacted or merged

with another, smaller galaxy.


M 83 (NGC 5236)

The M 83 subgroup

5º

Koribalski 2006Koribalski et al. In preparation


The galaxy NGC 5253

DHel= 4.0 Mpc (Karachentsev et al. 2004)

Scale: 19 pc / arcsec Optical size: 5.0’ 1.9’ Classified as Im pec, H II

starburst (NED), BCDG One of the closest

starbursts, observed at all wavelengths

It belongs to the M83 subgroup of the Centaurus Group

Deep analysis of its ionized gas using VLT López-Sánchez et al. 2007

NGC 5253 – B (blue) + V (green) + I (red) 2.5m du Pont telescope, Las Campanas Observatory, combined by Á.R. López-Sánchez

8.8’

NGC 5253 – V (blue) + I (green) + H (red) 2.5m du Pont telescope, LCO (V, I) + 1.5m CTIO (H) combined by Á.R. López-Sánchez


NGC 5253 VLA H I total intensity (contours) and optical image (gray image), Kobulnicky & Skillman, 1995, ApJ, 454, L121

NGC 5253: H I radio data

New radio data of NGC 5253 from the LVHIS project using three different ATCA arrays:

1.5A, 2x750A, EW367, no CA6. 6 km/s resolution, 32 channels Beam size: 86” 47”, PA 5º rms ~ 1.9 mJy /beam

NGC 5253 ATCA H I total intensity (false color) and DSS R optical image (contours)

Kobulnicky & Skillman, 1995


Total H I flux: ATCA: 31.1 1.5 Jy km/s VLA: 33.4 9.9 Jy km/s (Paturel et al. 2003)

H I mass: (8.0 0.4) 107 M

Dynamical mass: ~108 M


NGC 5253 – H I map (blue) + R (green) + H (red)



Optical major axis

Rotation?

NGC 5253 ATCA H I velocity field

H I velocity field:

Rotating about the optical MAJOR axis?


NGC 5253: H I radio data ESO 154-G023 ATCA H I velocity field

H I velocity field:

Rotating about the optical MAJOR axis? Any kind of outflow? Formation of a polar ring? Interaction with M83 ~1 Gyr ago? Disruption/accretion of a gas-rich companion?

See “Interactions and star formation activity in Wolf-Rayet galaxies” López-Sánchez PhD Thesis and Kobulnicky & Skillman 2008

H I velocity field:

Rotating about the optical MAJOR axis?


Dwarf galaxies

Comparison of H I and H properties

van Eymeren et al. 2008, in prep.

NGC 5408– D = 4.81 Mpc, IB(s)M– Opt. size = 2.6’ x 1.6’– H I size= 10’ x 6.3’– H I maxima coincide with

H II regions– H I mass: 3.2 108 M

– Fairly regular H I velocity field

IC 4662– D = 2.44 Mpc, BCDG– Opt. size = 3.0’ x 1.6’– H I size= 15’ x 12’– H I mass: 1.6 108 M

– Very distorted H I velocity field and intringuing H kinematics

Gaussian decomposition of the H I and H line shows outflows in both galaxies, with expansion velocities up to 75 km/s.









NGC 5408

IC 4662


Dwarf galaxies

















NGC 5408

IC 4662


The galaxy pair NGC 1512 / 1510The galaxy pair NGC 1512 / 1510

Central ring (16”x 12”) of NGC 1512 (HST, Maoz et al. 2001 )

NGC 1512: – SB(r)ab, Z ~0.7 Zo– D = 9.5 Mpc– Bar ~ 3’ = 8.3 kpc– Ring ~ 3’ x 2’

= 8.3 x 5.5 kpc– Nuclear ring ~ 16” x 12”

(740 x 550 pc) NGC 1510:

– S0, BCD, WR, Z~0.2 Zo– 5’ = 13.8 kpc

from NGC 1512 H images (Meurer et al.

2006) reveal many star forming regions

– Sizes 2” – 5” (90 – 230 pc)

– Dozens in the ring – NGC 1510– But also in external

regions with no evident continuum emission!



(740 x 550 pc) NGC 1510:

– S0, BCD, WR, Z~0.2 Zo– 5’ = 13.8 kpc

from NGC 1512 H images (Meurer et al.

2006) reveal many star forming regions

– Sizes 2” – 5” (90 – 230 pc)

– Dozens in the ring – NGC 1510– But also in external

regions with no evident continuum emission!



(740 x 550 pc)



(740 x 550 pc)


NGC 1512/1510 deep optical / UV imagesNGC 1512/1510 deep optical / UV images

Deep optical image (1.2 UKST, David Malin, priv. com.)

Deep optical image (1.2 UKST, David Malin, priv. com.)

Deep UV image (FUV + NUV, GALEX, Gil de Paz et

al. 2007)

Deep UV image (FUV + NUV, GALEX, Gil de Paz et

al. 2007)


NGC 1512 / 1510 – ATCA H I low resolution map

F HI = 268 Jy km/sM HI = 5.7 x 109 MoMHI / LB ~ 1

Between 1996 and 2005

7 arrays Mosaic using

4 pointings Total time:

4477 min (3.11 days)

Several H I maps:

–Low resolution, na-w, no CA06, b = 88.3” x 75.5”–Medium resolution, ro-w, no CA06, b = 62.1” x 55.3”–High resolution, ro-w, b = 13.0” x 11.3”

Several radio -continuum maps

Between 1996 and 2005

7 arrays Mosaic using

4 pointings Total time:

4477 min (3.11 days)

Several H I maps:

–Low resolution, na-w, no CA06, b = 88.3” x 75.5”–Medium resolution, ro-w, no CA06, b = 62.1” x 55.3”–High resolution, ro-w, b = 13.0” x 11.3”

Several radio -continuum maps

Koribalski, López-Sánchez & McIntyre, 2008, submitted


H I / UV comparison in NGC 1512/1510H I / UV comparison in NGC 1512/1510

SFR / Area increases with increasing M HI / Area

FUV – NUV color decreases with increasing M HI / Area

Places with higher HI column density have higher star formation activity and show younger ages

SFR / Area increases with increasing M HI / Area

FUV – NUV color decreases with increasing M HI / Area

Places with higher HI column density have higher star formation activity and show younger ages

Using GALEX images, we have derived UV colors and SFRs in individual UV-rich clusters and compare with HI distribution


NGC 1512 / 1510 – ATCA H I velocity field NGC 1512 / 1510 – ATCA H I velocity field


NGC 1512 / 1510 – ATCA H I velocity field NGC 1512 / 1510 – ATCA H I velocity field


NGC 1512 / 1510 Rotation fit and residues

NGC 1512 / 1510 Rotation fit and residues

The velocity field is mainly rotation,

But we found some discrepances in the most external regions and in the position of NGC 1510.

Star formation activity and the external HI structures seem to be consequence of the interaction that NGC 1512 and NGC 1510 are experiencing.

The velocity field is mainly rotation,

But we found some discrepances in the most external regions and in the position of NGC 1510.

Star formation activity and the external HI structures seem to be consequence of the interaction that NGC 1512 and NGC 1510 are experiencing.

Koribalski, López-Sánchez & McIntyre, 2008, subm.

NGC 1512 / 1510 also include in the THING project, with higher spatial resolution

(Deane & de Blok, in prep)

Koribalski, López-Sánchez & McIntyre, 2008, subm.

NGC 1512 / 1510 also include in the THING project, with higher spatial resolution

(Deane & de Blok, in prep)


ConclusionsConclusions LVHIS (Local Volume H I Survey) project is obtaining deep H I

and 20 cm radio-continuum imaging and of all nearby, gas-rich galaxies of the Local Volume (10 Mpc), so far +70 using the ATCA.

In order to understand:– H I distribution and environment,

– Kinematics and dynamics,

– Barionic and non-barionic matter distribution,

– Star formation properties on all scales.

Multiwavength comparison– Stellar distribution using

deep H-band images– Ionized gas distribution using H – UV (GALEX) and IR (SPITZER)

data when available

It is essential to know the properties of local galaxies in order to understand and to link with the properties of galaxies at higher redshifts (surveys at SKA & pathfinders).

LVHIS (Local Volume H I Survey) project is obtaining deep H I and 20 cm radio-continuum imaging and of all nearby, gas-rich galaxies of the Local Volume (10 Mpc), so far +70 using the ATCA.

In order to understand:– H I distribution and environment,

– Kinematics and dynamics,

– Barionic and non-barionic matter distribution,

– Star formation properties on all scales.

Multiwavength comparison– Stellar distribution using

deep H-band images– Ionized gas distribution using H – UV (GALEX) and IR (SPITZER)

data when available

It is essential to know the properties of local galaxies in order to understand and to link with the properties of galaxies at higher redshifts (surveys at SKA & pathfinders).

http://www.atnf.csiro.au/research/LVHIS

Documents

The Local Volume H I Survey