Detecting new supernova remnants with GLEAM Natasha Hurley-Walker - - PowerPoint PPT Presentation

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Detecting new supernova remnants with GLEAM Natasha Hurley-Walker - - PowerPoint PPT Presentation

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Detecting new supernova remnants with GLEAM Natasha Hurley-Walker Curtin University @ColourfulCosmos Supernova remnants Artists impression Credit: ESA/Hubble (L. Calada) 10 53 ergs gravitational energy Stars with M > 8M end in

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Detecting new supernova remnants with GLEAM

Natasha Hurley-Walker Curtin University

@ColourfulCosmos

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25th February 2019

Supernova remnants

  • Stars with M > 8MΘ end in core-collapse

supernovae (Type II, Ib/c)

  • White dwarfs disrupt binary companion, accrete,

supernova (Type Ia)

  • 1053 ergs gravitational energy
  • → 1051 kinetic energy deposited into stellar envelope
  • Ejected with v ~ 5000 km/s
  • Shock wave produces synchrotron and X-ray emission

Artist’s impression Credit: ESA/Hubble (L. Calçada)

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Impact on the interstellar medium

SN 1054 (Crab) SN 1006

  • p

t i c a l X

  • r

a y

  • Inject metals into the ISM, measurable

within our own solar system

(e.g. Vanhala & Boss 2002)

  • Disrupt star formation in nearby

molecular clouds

(e.g. Desai et al. 2010)

  • Heat ISM to 106 K
  • Fast shocks destroy H2

(Vanhala & Cameron 1998)

  • Slow shocks form CO, OH, H2O, CH+,

create and destroy dust grains

(see review: Sarangi 2018)

  • Accelerate cosmic rays at shock fronts

(Blandford & Ostriker 1978; Bell 1978; observational evidence e.g. Sano et al. 2018)

  • Some host pulsar wind nebulae

(PWNe)

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Radio morphologies

Dubner & Giacani 2015

Multi-shell Shell / barrel Blow-out Plerion Helical nebula

  • 95% of SNR detected via radio
  • Selection effects?
  • Resolution
  • Field-of-view / survey speed
  • Surface brightness sensitivity
  • Quality of ancillary IR data
  • Frequency of search
  • Bandwidth of search
  • 295 known (Green 2017)
  • Expect 3x more

(from O,B star counts, SN rates in Local Group, predicted synch lifetimes)

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Detecting radio supernova remnants

Brogan et al. (2006) Anderson et al. (2017)

Non-thermal: Radio emission Thermal: Radio+ infrared emission

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GaLactic and Extragalactic All-sky MWA survey

Publication highlights

  • Riseley et al. 2018: The POlarised GLEAM Survey (POGS) I: First Results from a Low-Frequency Radio Linear Polarisation Survey of the Southern Sky
  • For et al. 2018: A multifrequency radio continuum study of the Magellanic Clouds - I. Overall structure and star formation rates
  • Su et al. 2018: Galactic synchrotron distribution derived from 152 H II region absorption features in the full GLEAM survey
  • Galvin et al. 2018: The spectral energy distribution of powerful starburst galaxies - I. Modelling the radio continuum
  • Callingham et al 2017: Extragalactic Peaked-spectrum Radio Sources at Low Frequencies
  • George et al. 2017: A study of halo and relic radio emission in merging clusters using the Murchison Widefield Array
  • Kapinska et al. 2017: Spectral Energy Distribution and Radio Halo of NGC 253 at Low Radio Frequencies
  • Murphy et al. 2017: Low-Frequency Spectral Energy Distributions of Radio Pulsars Detected with the Murchison Widefield Array
  • Murphy et al. 2017: A search for long-time-scale, low-frequency radio transients
  • Su et al. 2017: Galactic synchrotron emissivity measurements between 250° < l < 355° from the GLEAM survey with the MWA
  • Hurley-Walker et al. 2017: GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey - I. A low-frequency extragalactic catalogue
  • Callingham et al. 2016: Low radio frequency observations and spectral modelling of the remnant of Supernova 1987A
  • Lenc et al. 2016: Low-frequency Observations of Linearly Polarized Structures in the Interstellar Medium near the South Galactic Pole
  • Hindson et al 2016: A Large-Scale, Low-Frequency Murchison Widefield Array Survey of Galactic H ii Regions between 260 < l < 340
  • Wayth et al. 2015: GLEAM: The GaLactic and Extragalactic All-Sky MWA Survey

Dec < 30º, 72 – 231 MHz, resolution ~ 2’, via 4 weeks with MWA 128T

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  • Images
  • gleam-vo.icrar.org or

SkyView

  • 8-MHz sub-bands from

72 – 231 MHz

  • Wideband 30 – 60 MHz

images

  • Catalogue
  • 307,455 sources
  • ~35mJy/beam flux limit
  • 20 flux densities
  • Spectral indices for

~70% of sources

GLEAM Data

Red = 72 – 103 MHz Green = 103 – 134 MHz Blue = 139 – 170 MHz

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Callingham et al. (2017)

  • Images
  • gleam-vo.icrar.org or

SkyView

  • 8-MHz sub-bands from

72 – 231 MHz

  • Wideband 30 – 60 MHz

images

  • Catalogue
  • 305,455 sources
  • ~35mJy/beam flux limit
  • 20 flux densities
  • Spectral indices for

~70% of sources

GLEAM Data

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(Current) Sky coverage

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Removed image artefacts Accurate flux calibration Better deconvolution

  • f large-scale

structure (Multiscale WSClean) Access to wider areas via improved peeling

GLEAM: Galactic Plane Imaging

BEFORE AFTER

Hurley-Walker et al. (submitted): GLEAM GP across 345° < l < 60°, 180° < l < 240°

RMS 10 – 20 mJy/beam @ 200MHz

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The GLEAM view of SNRs

GLEAM 200MHz

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The GLEAM view of SNRs

GLEAM 200MHz

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The GLEAM view of SNRs

GLEAM 200MHz GLEAM RGB (88/118/154)MHz

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The GLEAM view of SNRs

GLEAM 200MHz GLEAM RGB (88/118/154)MHz

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The GLEAM (and WISE) view of SNRs

22μm emission = thermal small dust grains 12μm emission = PAHs fluorescing from UV Widefield Infrared Survey Explorer (WISE) RGB (4.6/12/22)μm

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Measuring SNRs

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Following up SNR candidates

Green (2017)

  • 250 candidates
  • 136 in imaged region
  • 14 from MAGPIS
  • 101 from other sources

http://www.mrao.cam.ac.uk/surveys/snrs/snrs.info.html#S23

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Confirming candidates: G353.3-1.1

Parkes, 2.4 GHz (Duncan+95) GLEAM GP RGB α=-0.85, S200MHz~100Jy PSR → SNR diameter = 71pc → SNR age > 130,000 yr

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Understanding candidates:

GLEAM RGB (88/118/154)MHz MGPS (843 MHz) GLEAM 200MHz

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Understanding candidates: G3.1–0.7

GLEAM RGB (88/118/154)MHz MGPS (843 MHz) GLEAM 200MHz Blow-out VRO42.05.01

Landecker 1982

Density of ISM around A is 32x that around B

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Falsifying candidates: G19.00-0.35

Proposed by Gosachinski 1985 Clearly a (complex of) Hii region(s)! GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)μm GLEAM 200MHz

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Falsifying candidates: G19.00-0.35

See also Helfand et al. (2006): 31/49 candidates are actually HII regions GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)μm GLEAM 200MHz

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Submitted!

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345° < l < 60°

Known SNRs (green)

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345° < l < 60°

Known SNRs (green), known candidates (cyan), THOR candidates (red)

The HI/OH/RRL survey (Anderson+2017)

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Known SNRs (green), known candidates (cyan), THOR candidates (red), new candidates (magenta)

345° < l < 60°

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Known SNRs (green), known candidates (cyan), THOR candidates (red), new candidates (magenta)

180° < l < 240°

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27 new candidate SNRs

Filled

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New SNRs

Hurley-Walker et al. (submitted): New candidate SNRs from GLEAM

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A few compact SNR (<10’)

GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)um MGPS (843MHz) G 351.0 - 0.6

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Large, diffuse SNR

GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)um MGPS (843MHz) G 350.8 + 0.7

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Large, diffuse SNR

GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)um Effelsberg (2.7GHz) G 21.8+0.2

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Large, diffuse SNR

GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)um Effelsberg (2.7GHz) G 25.4-1.9

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High-latitude SNR

G 0.2-9.7 GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)um

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A new longitude range

.

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Pulsar associations

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G 0.2–9.7

J1825-33 (RRAT) DM = 43 ± 2 cm-3pc → Dist = 1.24 kpc → diameter = 24 pc SNR age estimate < 9k yr P = 1.27 s No P → no age estimate Position accuracy ~ 15’ → no kick velocity

Burke-Spolaor & Bailes 2010)

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G 21.8+0.2

J1831-0952 DM = 247 ± 5 cm-3pc → Dist = 3.68 kpc → diameter = 70 x 45 pc SNR age estimate ~ 40k – 120k yr P = 67 ms P = 8 x 10-15 s s-1 Age ~ 130k yr Kick velocity 170 – 490 km s-1

Lorimer et al. 2006

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G 230.5+1.3

J0729-1448 DM = 92 cm-3pc → Dist = 2.68 kpc → diameter = 47 x 31 pc SNR age estimate ~ 36k yr P = 252 ms P = 10-13 s s-1 Age ~ 35k yr Kick velocity 180 km s-1

Morris et al. (2002), Petroff et al. (2013)

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G 232.2+2.1

J0734-1559 (γ-ray pulsar) No DM → No Dist → No diameter → No SNR age estimate P = 155 ms P = 10-14 s s-1 Age ~ 200k yr

Sokolova & Rubstov (2016)

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New pulsars?

G 350.8+5.1 Compact source α=-1.4 Pulsar? GLEAM RGB (88/118/154)MHz WISE RGB (8/12/22)um

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Comparisons with known SNR (Green 2017)

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GLEAM-eXtended

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GLEAM-eXtended

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GLEAM-eXtended

GLEAM 170 – 231 MHz RMS: ~7 mJy/beam Resolution: 2’ GLEAM-X 170 – 231 MHz RMS: ~2 mJy/beam Resolution: 1’ GLEAM-X Red = 72 – 103 MHz Green = 103 – 134 MHz Blue = 139 – 170 MHz

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With these powers combined...

GLEAM 72 – 103 MHz Resolution: 2’ Feathered combination MWA Phase II 72 – 103 MHz Resolution: 1’ (Credit: Chenoa Tremblay)

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