Arecibo radio astronomy
Download
1 / 32

ARECIBO RADIO ASTRONOMY - PowerPoint PPT Presentation


  • 117 Views
  • Uploaded on

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

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' ARECIBO RADIO ASTRONOMY' - shamus


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
Arecibo radio astronomy
ARECIBO RADIO ASTRONOMY

Chris Salter for Murray Lewis

11 September 2008 NSF


Across whole arecibo pgm
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
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

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
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




Traditional arecibo topics1
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
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


Btf from resolved rotation curves

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
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
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



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

11 September 2008 NSF


Text Catinella et al ApJL

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

11 September 2008 NSF


HIMF Catinella et al ApJL

  • 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 Catinella et al ApJL


11 September 2008 NSF Catinella et al ApJL


Traditional arecibo topics2
Traditional Arecibo topics Catinella et al ApJL

  • 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 Catinella et al ApJL

Dec. 21 - 26°; RA 3hr - 23 hr

11 September 2008 NSF


11 September 2008 NSF Catinella et al ApJL


11 September 2008 NSF Catinella et al ApJL


Magnetic fields
Magnetic Fields Catinella et al ApJL

GALFACTS

11 September 2008 NSF


11 September 2008 NSF Catinella et al ApJL


Vlbi and arecibo the impact of arecibo s sensitivity
VLBI and Arecibo Catinella et al ApJLThe 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 Catinella et al ApJL

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
Exploiting 1 - 10 GHz Catinella et al ApJL

  • 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
A Spectral Scan of Arp 220: Catinella et al ApJL1.1 – 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
The Spectrum of Arp 220 – Prebiotic Molecules Catinella et al ApJL

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 Catinella et al ApJL


ad