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ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez The Local Volume H I Survey Ángel R. López-Sánchez Ángel R. López-Sánchez Bärbel S. Koribalski & the.

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Presentation on theme: "ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez The Local Volume H I Survey Ángel R. López-Sánchez Ángel R. López-Sánchez Bärbel S. Koribalski & the."— Presentation transcript:

1 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez The Local Volume H I Survey Ángel R. López-Sánchez Ángel R. López-Sánchez Bärbel S. Koribalski & the LVHIS team Ángel R. López-Sánchez Ángel R. López-Sánchez Bärbel S. Koribalski & the LVHIS team CSIRO /Australia Telescope National Facility (ATNF, Australia) Gas and Stars in Galaxies: A Multi-Wavelength 3D Perspective ESO Workshop – Garching – 10 Jun 2008 CSIRO /Australia Telescope National Facility (ATNF, Australia) Gas and Stars in Galaxies: A Multi-Wavelength 3D Perspective ESO Workshop – Garching – 10 Jun 2008

2 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez Galaxies in the Local Volume Local Volume: 10 Mpc ( v LG < 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 ( v LG < 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 (based on 450 LV galaxies with D < 10 Mpc) M83 and CenA groupings M81 and IC342 groupings Sculptor group

3 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez Galaxies in the Local Volume Local Volume: 10 Mpc ( v LG < 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 ( v LG < 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 (based on 450 LV galaxies with D < 10 Mpc) HIPASS LVHIS HIPASS: H I Parkes All Sky Survey LVHIS: +70 galaxies from the ATCA

4 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez LVHIS observations Deep H I line & 20 cm radio continuum observations for all nearby (v LG < 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 cm -2 (for 60” beam) – Expand to GMRT, VLA, WSRT Deep H I line & 20 cm radio continuum observations for all nearby (v LG < 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 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)  COMPLETE NOW!

5 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez LVHIS objectives Deep H I imaging of all nearby, gas-rich galaxies – Integrated HI distribution galaxy diameters, asymmetries, tidal tails, companions – Mean HI velocity field V rot (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 V rot (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 AM0319–662 NGC 253 NGC 5253 NGC cm cont + R image IC 5052 H I map (blue) + H (green) + H  (red) (Kirby et al. 2008) NGC cm cont + R image IC 5052 H I map (blue) + H (green) + H  (red) (Kirby et al. 2008)

6 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez HI and total mass distribution in the Local Volume HI mass function & optical luminosity function HI vs optical diameter M HI /L B, M HI /L H 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 M HI /L B, M HI /L H 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 Science

7 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', D cepheid – 4.5 ± 0.3 Mpc. UGCA 365 Visible (8.2m VLT) H I map ATCA mosaic, Koribalski et al, in p. – M HI = 8  10 9 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.

8 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez M 83 (NGC 5236)

9 The M 83 subgroup 5º Koribalski 2006 Koribalski et al. In preparation

10 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez The galaxy NGC 5253 D Hel = 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 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

11 ESO Workshop – Jun 10, 2008 Ángel 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

12 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez 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)  10 7 M  Dynamical mass: ~10 8 M  NGC 5253: H I radio data NGC 5253 – H I map (blue) + R (green) + H  (red)

13 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez NGC 5253: H I radio data Optical major axis Rotation? NGC 5253 ATCA H I velocity field H I velocity field: Rotating about the optical MAJOR axis?

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

15 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez 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  10 8 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  10 8 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. 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  10 8 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  10 8 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

16 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez 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  10 8 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  10 8 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. 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  10 8 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  10 8 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

17 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez The galaxy pair NGC 1512 / 1510 Central ring (16”x 12”) of NGC 1512 (HST, Maoz et al ) 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! 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! 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 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)

18 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez NGC 1512/1510 deep optical / UV images Deep optical image (1.2 UKST, David Malin, priv. com.) Deep UV image (FUV + NUV, GALEX, Gil de Paz et al. 2007)

19 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez NGC 1512 / 1510 – ATCA H I low resolution map F HI = 268 Jy km/s M HI = 5.7 x 10 9 Mo M HI / L B ~ 1 Between 1996 and 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 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

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

23 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez NGC 1512 / 1510 – ATCA H I velocity field

24 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez NGC 1512 / 1510 – ATCA H I velocity field

25 ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez 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 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 Star formation activity and the external HI structures seem to be consequence of the interaction that NGC 1512 and NGC 1510 are experiencing. Further analysi s (i.e., includi ng numeri cal simulat ions) will quantif y the importa nce of such interact ion. 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)

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

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