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ARECIBO RADIO ASTRONOMY. Chris Salter for Murray Lewis. Across whole Arecibo pgm. Mass -range investigated dynamically ~56 orders of magnitude Micro-meteorites -- asteroids -- neutron stars -- -- galaxy clusters Time duration: ∆t > 23 orders of magnitude

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ARECIBO RADIO ASTRONOMY

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ARECIBO RADIO ASTRONOMY

Chris Salter for Murray Lewis

11 September 2008 NSF


Across whole Arecibo pgm.

  • Mass-range investigated dynamically

    • ~56 orders of magnitude

    • Micro-meteorites -- asteroids -- neutron stars -- -- galaxy clusters

  • Time duration: ∆t > 23 orders of magnitude

    • Crab giant pulses 10-9 sec; Galaxy Evoln. > 109 yr

  • Magnetic field: B > 20 orders of magnitude

    • Mercury null; ISM; to Magnetars > 10^13 gauss

11 September 2008 NSF


Traditional Arecibo topics

  • Pulsars -- (pALFA), timing MSP

  • 21 cm HI

    • Extra-galactic {alfalfa, AGES, (AUDS), ([ZoA]) }

    • Galactic {Disk-Halo, (I-gALFA), [TOGS,TOGS2,GALFACTS2]}

  • OTHER

    • Magnetic Fields {(GALFACTS), (ULIRGs) }

    • VLBI

    • Multi-UGC, CGCG, SDSS, IRAS, 2MASS, (GLAST)}

    • Molecular-line {Arp 220, ULIRGs}

11 September 2008 NSF


ALFA: A Camera for Arecibo

  • Installed 2004 Apr

  • Surveys initiated Feb 2005

  • 7 beams x 2 pol (linear) = 14 “pixels”

  • 1225-1525 MHz full range

  • Unmatched sensitivity (SEFD = 2.4 to 3 Jy)

  • 3.3’ x 3.8’ beams on 11’ X 13’ ellipse

  • Unprecedented capability for mapping the sky

  • Survey consortia self-organized by community

2004

11 September 2008 NSF


Pulsars

  • Discovery -- (pALFA)

  • timing, MSP timing, gravitational-waveenergy density

  • timing noise investigations

  • high-time resolution studies

  • tests of general relativity

  • physics of extreme environments (B, Eqn. State)

  • ISM studies (using pulsars as probes of ISM, etc)

  • precision astrometry (parallaxes, proper motions, etc)

  • pulsar time scales (inertial & dynamical)

11 September 2008 NSF


2.15 msec

95 d orbit

e 0.43667

1.74±0.04 Mo

J1903+0327

11 September 2008 NSF


11 September 2008 NSF


11 September 2008 NSF


Traditional Arecibo topics

  • Pulsars -- (pALFA), timing MSP

  • 21 cm HI

    • Extra-galactic {alfalfa, AGES, (AUDS), ([ZoA]) }

    • Galactic {Disk-Halo, (I-gALFA), [TOGS,TOGS2,GALFACTS2]}

  • OTHER

    • Magnetic Fields {(GALFACTS), (ULIRGs) }

11 September 2008 NSF


HI STUDIES

  • Trace phase change from ionized to neutral species

  • HI eliminated via phase change to molecular species

  • Traces accumulation of visible baryons into galaxies -- Tully Fisher Relation

11 September 2008 NSF


300

200

V, km/s

100

30

10

50

r, kpc

BTF from Resolved Rotation Curves

M33

stars

HI

Need aperture synthesis HI maps - limits sample sizes

HI

H

Vrot

h

d

b

HI

KS 2005

NRAO/AUI and NOAO/AURA/NSF

Rector et al.

11 September 2008 NSF


The Baryonic Tully-Fisher Relation

BTF

Stellar TF

1011

1011

H

K’

I

B

Md

M*

(Mo)

(Mo)

109

109

(colors)

107

107

McGaugh et al 2000

30

100

300

100

300

30

Vrot (km/s)

Vrot (km/s)

Philosophy

Coverage over Completeness

11 September 2008 NSF


Arecibo as an HI telescope

in the coming era of active SKA survey- optimized pathfinders (ASKAP, MSKAP)

to be followed by the SKA

whence Arecibo?

The mid-range SKA is a 0.3-3 GHz+ facility

That exactly matches Arecibo, so

Arecibo’s scienceis SKA precursor science

11 September 2008 NSF


Exploit Sensitivity by

  • Looking at large redshifts

    => evolution in TF relation

  • Looking for local very low mass objects

    => alfalfa

11 September 2008 NSF


11 September 2008 NSF


A Pilot Survey of HI in Field Galaxies at z ~ 0.2: Catinella et al ApJL

11 September 2008 NSF


Text

~5300 galaxies from alfalfa: RA 7.5 - 16.5 hr, dec 12 - 16°

11 September 2008 NSF


HIMF

  • Previous surveys have detected few (if any) objects with low HI.

  • At low mass end, HIMF estimates differ by >10X:

    • Rosenberg & Schneider (2000)

    • versus

    • Zwaan et al. (1997)

?

Parkes HIPASS survey: Zwaan et al. 2003

11 September 2008 NSF


11 September 2008 NSF


11 September 2008 NSF


Traditional Arecibo topics

  • Pulsars -- (pALFA), timing MSP

  • 21 cm HI

    • Extra-galactic {alfalfa, AGES, (AUDS), ([ZoA]) }

    • Galactic {Disk-Halo, (I-gALFA), [TOGS,TOGS2,GALFACTS2]}

  • OTHER

    • Magnetic Fields {(GALFACTS), (ULIRGs) }

11 September 2008 NSF


TOGS HI map from commensal observations in fall 2007

Dec. 21 - 26°; RA 3hr - 23 hr

11 September 2008 NSF


11 September 2008 NSF


11 September 2008 NSF


Magnetic Fields

GALFACTS

11 September 2008 NSF


11 September 2008 NSF


VLBI and AreciboThe impact of Arecibo’s sensitivity

  • Arecibo added to the VLBA => 4.5 times better sensitivity (Day & Momjian 2005).

11 September 2008 NSF


VLBI Highlights Post-Painting

MK5A Disk-recorded:Three successful Mk5A disk-based runs using L, C and

X-band, with HAS, EVN & Global network. These represent; (1) a study of the Zeeman effect for compact components in ULIRGs, (2) jet and counter-jet emission in the giant radio galaxy, NGC315 and, (3) measuring the expansion velocity of SN2008D associated with the transient X-ray source in NGC2770 (Target of Opportunity).

E-VLBI test over the existing OC3 (155Mbps-shared with UPR) line:

Arecibo data arriving at JIVE

Fringe amplitude for 128 Mbps

@128Mbps

@64Mbps

Jb - Tr

Jb - Wb

Fringe amplitude for 64Mbps

Jb - Tr

Jb - Wb

Jb - Ar

Tr - Wb

Jb - Ar

Tr - Wb

QSO 3C395

Tr - Ar

Wb - Ar

Wb - Ar

Tr - Ar

11 September 2008 NSF


Exploiting 1 - 10 GHz

  • Molecular line searches (Galactic starting)

  • Molecular line searches extragalactic

    ULIRGS, recent success

11 September 2008 NSF


A Spectral Scan of Arp 220:1.1 – 10 GHz

Arp 220 is a star-burst galaxy at a distance of 250 Mly.

It is forming stars at 100-times the rate of the Milky Way.

It is the result of a collision between 2 galaxies now in the final stages of merging.

(VLA:Radio

Wavlength 6cm)‏

(HST:Optical)‏

11 September 2008 NSF


The Spectrum of Arp 220 – Prebiotic Molecules

Methanimine (CH2NH) observed for the first time outside of the Milky Way (where it has only been observed in one source!)‏

This is probably a maser emitter.

“Bending” transitions of HCN observed for the very first time in the radio region.

These lines are at L-, C-, C-Hi & X-band.

STOP PRESS:

HCN at S-band.

11 September 2008 NSF


11 September 2008 NSF


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