A MeerKAT survey of nearby nova-like cataclysmic variables

D. M. Hewitt; M. L. Pretorius; P. A. Woudt; E. Tremou; J. C.A. Miller-Jones; C. Knigge; N. Castro Segura; D. R.A. Williams; R. P. Fender; R. Armstrong; P. Groot; I. Heywood; A. Horesh; A. J. Van Der Horst; E. Koerding; V. A. McBride; K. P. Mooley; A. Rowlinson; B. Stappers; R. A.M.J. Wijers

doi:10.1093/mnras/staa1747

A MeerKAT survey of nearby nova-like cataclysmic variables

D. M. Hewitt^*, M. L. Pretorius, P. A. Woudt, E. Tremou, J. C.A. Miller-Jones, C. Knigge, N. Castro Segura, D. R.A. Williams, R. P. Fender, R. Armstrong, P. Groot, I. Heywood, A. Horesh, A. J. Van Der Horst, E. Koerding, V. A. McBride, K. P. Mooley, A. Rowlinson, B. Stappers, R. A.M.J. Wijers

^*Corresponding author for this work

Racah Institute of Physics

Research output: Contribution to journal › Review article › peer-review

11 Scopus citations

Abstract

We present the results of MeerKAT radio observations of 11 nearby nova-like cataclysmic variables (CVs). We have detected radio emission from IM Eri, RW Sex, V3885 Sgr, and V603 Aql. While RW Sex, V3885 Sgr, and V603 Aql had been previously detected, this is the first reported radio detection of IM Eri. Our observations have doubled the sample of non-magnetic CVs with sensitive radio data. We observe that at our radio detection limits, a specific optical luminosity ≳2.2× 1018 erg s-1 Hz-1 (corresponding to MV ≲ 6.0) is required to produce a radio detection. We also observe that the X-ray and radio luminosities of our detected nova-like CVs are on an extension of the LXλ LR∼ 0.7 power law originally proposed for non-pulsating neutron star low-mass X-ray binaries. We find no other correlations between the radio emission and emission in other wavebands or any other system parameters for the existing sample of radio-detected non-magnetic CVs. We measure in-band (0.9-1.7 GHz) radio spectral indices that are consistent with reports from earlier work. Finally, we constructed broad spectral energy distributions for our sample from published multiwavelength data, and use them to place constraints on the mass transfer rates of these systems.

Original language	American English
Pages (from-to)	2542-2557
Number of pages	16
Journal	Monthly Notices of the Royal Astronomical Society
Volume	496
Issue number	3
DOIs	https://doi.org/10.1093/mnras/staa1747
State	Published - 17 Jun 2020

Bibliographical note

Funding Information:
DMH acknowledges financial support from the National Research Foundation (NRF) and the South African Astronomical Observatory (SAAO). PAW kindly acknowledges financial support from the University of Cape Town and the NRF. MLP acknowledges financial support from the NRF and the Newton Fund. JCAM-J is the recipient of an Australian Research Council Future Fellowship (FT140101082), funded by the Australian government. This work was supported by the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation.

Funding Information:
This publication has used data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by NASA.

Funding Information:
This work has used data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https:// www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Funding Information:
This publication has used data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation.

Publisher Copyright:
© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.

Keywords

X-rays: binaries
accretion, accretion discs
novae, cataclysmic variables
radio continuum: stars
stars: jets
white dwarfs

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10.1093/mnras/staa1747

Cite this

Hewitt, D. M., Pretorius, M. L., Woudt, P. A., Tremou, E., Miller-Jones, J. C. A., Knigge, C., Castro Segura, N., Williams, D. R. A., Fender, R. P., Armstrong, R., Groot, P., Heywood, I., Horesh, A., Van Der Horst, A. J., Koerding, E., McBride, V. A., Mooley, K. P., Rowlinson, A., Stappers, B., & Wijers, R. A. M. J. (2020). A MeerKAT survey of nearby nova-like cataclysmic variables. Monthly Notices of the Royal Astronomical Society, 496(3), 2542-2557. https://doi.org/10.1093/mnras/staa1747

@article{5f254b2932464b78ae36a00feb695d39,

title = "A MeerKAT survey of nearby nova-like cataclysmic variables",

abstract = "We present the results of MeerKAT radio observations of 11 nearby nova-like cataclysmic variables (CVs). We have detected radio emission from IM Eri, RW Sex, V3885 Sgr, and V603 Aql. While RW Sex, V3885 Sgr, and V603 Aql had been previously detected, this is the first reported radio detection of IM Eri. Our observations have doubled the sample of non-magnetic CVs with sensitive radio data. We observe that at our radio detection limits, a specific optical luminosity ≳2.2× 1018 erg s-1 Hz-1 (corresponding to MV ≲ 6.0) is required to produce a radio detection. We also observe that the X-ray and radio luminosities of our detected nova-like CVs are on an extension of the LXλ LR∼ 0.7 power law originally proposed for non-pulsating neutron star low-mass X-ray binaries. We find no other correlations between the radio emission and emission in other wavebands or any other system parameters for the existing sample of radio-detected non-magnetic CVs. We measure in-band (0.9-1.7 GHz) radio spectral indices that are consistent with reports from earlier work. Finally, we constructed broad spectral energy distributions for our sample from published multiwavelength data, and use them to place constraints on the mass transfer rates of these systems.",

keywords = "X-rays: binaries, accretion, accretion discs, novae, cataclysmic variables, radio continuum: stars, stars: jets, white dwarfs",

author = "Hewitt, {D. M.} and Pretorius, {M. L.} and Woudt, {P. A.} and E. Tremou and Miller-Jones, {J. C.A.} and C. Knigge and {Castro Segura}, N. and Williams, {D. R.A.} and Fender, {R. P.} and R. Armstrong and P. Groot and I. Heywood and A. Horesh and {Van Der Horst}, {A. J.} and E. Koerding and McBride, {V. A.} and Mooley, {K. P.} and A. Rowlinson and B. Stappers and Wijers, {R. A.M.J.}",

note = "Funding Information: DMH acknowledges financial support from the National Research Foundation (NRF) and the South African Astronomical Observatory (SAAO). PAW kindly acknowledges financial support from the University of Cape Town and the NRF. MLP acknowledges financial support from the NRF and the Newton Fund. JCAM-J is the recipient of an Australian Research Council Future Fellowship (FT140101082), funded by the Australian government. This work was supported by the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. Funding Information: This publication has used data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by NASA. Funding Information: This work has used data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https:// www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Funding Information: This publication has used data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation. Publisher Copyright: {\textcopyright} 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.",

year = "2020",

month = jun,

day = "17",

doi = "10.1093/mnras/staa1747",

language = "American English",

volume = "496",

pages = "2542--2557",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Hewitt, DM, Pretorius, ML, Woudt, PA, Tremou, E, Miller-Jones, JCA, Knigge, C, Castro Segura, N, Williams, DRA, Fender, RP, Armstrong, R, Groot, P, Heywood, I, Horesh, A, Van Der Horst, AJ, Koerding, E, McBride, VA, Mooley, KP, Rowlinson, A, Stappers, B & Wijers, RAMJ 2020, 'A MeerKAT survey of nearby nova-like cataclysmic variables', Monthly Notices of the Royal Astronomical Society, vol. 496, no. 3, pp. 2542-2557. https://doi.org/10.1093/mnras/staa1747

TY - JOUR

T1 - A MeerKAT survey of nearby nova-like cataclysmic variables

AU - Hewitt, D. M.

AU - Pretorius, M. L.

AU - Woudt, P. A.

AU - Tremou, E.

AU - Miller-Jones, J. C.A.

AU - Knigge, C.

AU - Castro Segura, N.

AU - Williams, D. R.A.

AU - Fender, R. P.

AU - Armstrong, R.

AU - Groot, P.

AU - Heywood, I.

AU - Horesh, A.

AU - Van Der Horst, A. J.

AU - Koerding, E.

AU - McBride, V. A.

AU - Mooley, K. P.

AU - Rowlinson, A.

AU - Stappers, B.

AU - Wijers, R. A.M.J.

N1 - Funding Information: DMH acknowledges financial support from the National Research Foundation (NRF) and the South African Astronomical Observatory (SAAO). PAW kindly acknowledges financial support from the University of Cape Town and the NRF. MLP acknowledges financial support from the NRF and the Newton Fund. JCAM-J is the recipient of an Australian Research Council Future Fellowship (FT140101082), funded by the Australian government. This work was supported by the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. Funding Information: This publication has used data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by NASA. Funding Information: This work has used data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https:// www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Funding Information: This publication has used data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation. Publisher Copyright: © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.

PY - 2020/6/17

Y1 - 2020/6/17

N2 - We present the results of MeerKAT radio observations of 11 nearby nova-like cataclysmic variables (CVs). We have detected radio emission from IM Eri, RW Sex, V3885 Sgr, and V603 Aql. While RW Sex, V3885 Sgr, and V603 Aql had been previously detected, this is the first reported radio detection of IM Eri. Our observations have doubled the sample of non-magnetic CVs with sensitive radio data. We observe that at our radio detection limits, a specific optical luminosity ≳2.2× 1018 erg s-1 Hz-1 (corresponding to MV ≲ 6.0) is required to produce a radio detection. We also observe that the X-ray and radio luminosities of our detected nova-like CVs are on an extension of the LXλ LR∼ 0.7 power law originally proposed for non-pulsating neutron star low-mass X-ray binaries. We find no other correlations between the radio emission and emission in other wavebands or any other system parameters for the existing sample of radio-detected non-magnetic CVs. We measure in-band (0.9-1.7 GHz) radio spectral indices that are consistent with reports from earlier work. Finally, we constructed broad spectral energy distributions for our sample from published multiwavelength data, and use them to place constraints on the mass transfer rates of these systems.

AB - We present the results of MeerKAT radio observations of 11 nearby nova-like cataclysmic variables (CVs). We have detected radio emission from IM Eri, RW Sex, V3885 Sgr, and V603 Aql. While RW Sex, V3885 Sgr, and V603 Aql had been previously detected, this is the first reported radio detection of IM Eri. Our observations have doubled the sample of non-magnetic CVs with sensitive radio data. We observe that at our radio detection limits, a specific optical luminosity ≳2.2× 1018 erg s-1 Hz-1 (corresponding to MV ≲ 6.0) is required to produce a radio detection. We also observe that the X-ray and radio luminosities of our detected nova-like CVs are on an extension of the LXλ LR∼ 0.7 power law originally proposed for non-pulsating neutron star low-mass X-ray binaries. We find no other correlations between the radio emission and emission in other wavebands or any other system parameters for the existing sample of radio-detected non-magnetic CVs. We measure in-band (0.9-1.7 GHz) radio spectral indices that are consistent with reports from earlier work. Finally, we constructed broad spectral energy distributions for our sample from published multiwavelength data, and use them to place constraints on the mass transfer rates of these systems.

KW - X-rays: binaries

KW - accretion, accretion discs

KW - novae, cataclysmic variables

KW - radio continuum: stars

KW - stars: jets

KW - white dwarfs

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U2 - 10.1093/mnras/staa1747

DO - 10.1093/mnras/staa1747

M3 - Review article

AN - SCOPUS:85089798202

SN - 0035-8711

VL - 496

SP - 2542

EP - 2557

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

A MeerKAT survey of nearby nova-like cataclysmic variables

Abstract

Bibliographical note

Keywords

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