Observations of extragalactic neutral hydrogen
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Observations of Extragalactic Neutral Hydrogen. Spencer Wolfe Kristina Nyland Laura Trouille Blakesley Burkhart Robert Minchin. Why observe the 21 cm line in other galaxies?. Center of line provides recessional velocity of galaxy provides distance to galaxy (if unknown) Width of line

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Observations of extragalactic neutral hydrogen

Observations of Extragalactic Neutral Hydrogen

Spencer Wolfe

Kristina Nyland

Laura Trouille

Blakesley Burkhart

Robert Minchin


Why observe the 21 cm line in other galaxies
Why observe the 21 cm line in other galaxies?

  • Center of line

    • provides recessional velocity of galaxy

    • provides distance to galaxy (if unknown)

  • Width of line

    • provides rotational velocity of the galaxy

    • provides dynamical mass of the galaxy

  • Total flux in HI line

    • provides HI mass of the galaxy

    • probes correlations with optical galaxy morphology, dynamical mass, IR flux, and variations with redshift

Above: The Circinus spiral galaxy mapped in HI by the ATCA. The left and right sides represent (respectively) the moment 0 (integrated flux) and the moment 1 (velocity).


Instrument set up
Instrument Set-up

  • L-band receiver (centered at 1420.406 MHz)

  • Filter at 1370-1470 MHz

  • Backend: WAPP correlator (25-50 MHz)

  • Standard on/off observing mode

  • 8 galaxies observed in 2 hours

    • all galaxies chosen w/ velocities < 10,000 km/s

    • 300 sec integration time per target


Let s play guess the profile
Let’s Play ‘Guess the Profile’

NGC 6021

NGC 5996

Spiral (SBc, starburst)

Elliptical

First 21-cm detection of NGC 6021 !


Ugc 10281 sb s m z 0 03
UGC 10281, SB(s)m, z~0.03

M(HI) = 3.8e8

Mdyn = 2.3e10


Arms?

CGCG 082-035

M(HI) = 1.4e9

Mdyn = 7.5e9

Unknown classification in NED,

found in 2MASS survey

M(HI) = 9.7e8

Mdyn = 4.5e9

UGC 10805

SBm


M(HI) = 1.4e9

Mdyn = 4.7e10

UGC 10841

Sdm

M(HI) = 3.6e8

Mdyn = 8.5e10

IC 1135

Sa

i=30 deg


Mass ratios
Mass Ratios

1) HI in looser spirals tends to account for a greater portion of their total mass.

2) Tighter spiral and elliptical have a lower fraction of HI compared to their total mass.

3) This supports the general view of spiral vs elliptical galaxy characteristics.


Acknowledgements
Acknowledgements

We would like to thank Robert Minchin for his help with observing and reducing our data. Thanks Robert!


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