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Swift Nova-CV Group

Members of the Nova-CV exploder list ()

Presentations

Swift Cataclysmic Variables and Novae - "What Next for Swift?" Meeting (1-2 May 2007)
Classical Novae in the Swift Era - HEAD 2008
Swift X-ray and UV Observations of Novae - Stella Novae: Past and Future Decades (2013)

Swift nova papers with involvement by the group

• V392 Per
  • V392 Persei: A γ-ray bright nova eruption from a known dwarf nova
    Murphy-Glaysher et al., 2022, MNRAS, 514, 6183
• YZ Ret
  • Mixing of Hot Shocked Plasma with Cold Gas in Nova YZ Ret 2020
    Mitrani et al., 2024, ApJ, 970, 54
  • The first nova eruption in a novalike variable: YZ Ret as seen in X-rays and γ-rays
    Sokolovsky et al., 2022, MNRAS, 514, 2239
• V1674 Her
  • Soft X-ray and FUV observations of Nova Her 2021 (V1674 Her) with AstroSat
    Bhargava et al., 2024, MNRAS, 528, 28
  • The multiwavelength view of shocks in the fastest nova V1674 Her
    Sokolovsky et al., 2023, MNRAS, 521, 5453
  • The Remarkable Spin-down and Ultra-fast Outflows of the Highly-Pulsed Supersoft Source of Nova Herculis 2021
    Drake et al., 2021, 922, L42
  • Near-infrared studies of nova V1674 Herculis: A shocking record-breaker
    Woodward et al., 2021, ApJ, 922, L10
• V3890 Sgr
  • The Super-Soft Source Phase of the recurrent nova V3890 Sgr
    Ness et al., 2022, A&A, 658, A169
  • AstroSat soft X-ray observations of the symbiotic recurrent nova V3890 Sgr during its 2019 outburst
    Singh et al., 2021, MNRAS, 501, 36
  • The 2019 eruption of recurrent nova V3890 Sgr: observations by Swift, NICER, and SMARTS
    Page et al., 2020, MNRAS, 499, 4814
  • Chandra High Energy Transmission Gratings Spectra of V3890 Sgr
    Orio et al., 2020, ApJ, 895, 80
• V906 Car
  • X-ray Spectroscopy of the gamma-ray Brightest Nova V906 Car (ASASSN-18fv)
    Sokolovsky et al., 2020, MNRAS, 497, 2569
  • Direct evidence for shock-powered optical emission in a nova
    Aydi et al., 2020, NatAs, 4, 776
• Nova LMC 1968
  • Near-infrared spectroscopy of the LMC recurrent nova LMCN 1968-12a
    Evans et al., 2025, MNRAS, 536, 1710
  • Similarities between the X-Ray Light Curves of the 2016 and 2020 Eruptions of the Recurrent Nova LMC 1968
    Schwarz, Page, Kuin & Darnley, 2020, RNAAS, 4, 142
  • The 2016 January eruption of recurrent Nova LMC 1968
    Kuin et al., 2020, MNRAS, 491, 655
• V407 Lup
  • Multiwavelength observations of V407 Lupi (ASASSN-16kt) - a very fast nova erupting in an intermediate polar
    Aydi et al., 2018, MNRAS, 480, 572
• V5668 Sgr
  • A two-component clumpy model for the shell evolution of classical novae: the case of V5668 Sgr
    Abraham et al., 2024, MNRAS, 527, 7482
  • The Temporal Development of Dust Formation and Destruction in Nova Sagittarii 2015#2 (V5668 Sgr): A Panchromatic Study
    Gehrz et al., 2018, ApJ, 858, 78
• Nova SMC 2016
  • What We Learn from the X-Ray Grating Spectra of Nova SMC 2016
    Orio et al., 2018, ApJ, 862, 164
  • Multiwavelength observations of nova SMCN 2016-10a --- one of the brightest novae ever observed
    Aydi et al., 2018, MNRAS, 474, 2679
• V339 Del
  • The panchromatic spectroscopic evolution of the classical CO nova V339 Delphini (Nova Del 2013) until X-ray turnoff
    Shore et al., 2016, A&A, 590, A123
• Nova LMC 2009a
  • Pan-Chromatic observations of the Recurrent Nova LMC 2009a (LMC 1971b)
    Bode et al., 2016, ApJ, 818, 145
• Nova LMC 2012
  • Pan-Chromatic Observations of the Remarkable Nova Large Magellanic Cloud 2012
    Schwarz et al., 2015, AJ, 149, 95
• V745 Sco
  • Collimation and Asymmetry of the Hot Blast Wave from the Recurrent Nova V745 Sco
    Drake, J.J. et al., 2016, ApJ, 825, 95
  • Swift detection of the super-swift switch-on of the super-soft phase in nova V745 Sco (2014)
    Page et al., 2015, MNRAS, 454, 3108
  • A NuSTAR observation of the fast symbiotic nova V745 Sco in outburst
    Orio et al., 2015, MNRAS, 448, L35
• U Sco
  • Infrared spectroscopy of the 2022 eruption of the recurrent nova U Sco
    Evans et al., 2023, MNRAS, 522, 4841
  • The 2010 Eruption of the Recurrent Nova U Scorpii: The Multi-wavelength Light Curve
    Pagnotta et al., 2015, ApJ, 811, 32
• M31N 2008-12a
  • Near-infrared spectroscopy of the recurrent nova M31N 2008-12a
    Banerjee et al., 2025, MNRAS, 540, 1780
  • Breaking the habit - the peculiar 2016 eruption of the unique recurrent nova M31N 2008-12a
    Henze et al., 2018, ApJ, 857, 68
  • M31N 2008-12a - The Remarkable Recurrent Nova in M31: Panchromatic Observations of the 2015 Eruption.
    Darnley et al., 2016, ApJ, 833, 149
  • X-ray Flashes in Recurrent Novae: M31N 2008-12a and the Implications of the Swift Nondetection
    Kato et al., 2016, ApJ, 830, 40
  • A remarkable recurrent nova in M 31: The predicted 2014 outburst in X-rays with Swift
    Darnley et al., 2015, A&A, 580, A46
  • A remarkable recurrent nova in M31: Discovery and optical/UV observations of the predicted 2014 eruption
    Henze et al., 2015, A&A, 580, A45
  • A remarkable recurrent nova in M 31: The X-ray observations
    Henze et al., 2014, A&A, 563, L8
• Nova Mon 2012
  • The 7.1 hour X-ray-UV-NIR period of the gamma-ray classical Nova Monocerotis 2012
    Page et al., 2013, ApJ, 768, L26
• HV Cet (CSS 081007:030559+054715)
  • The outburst of Nova CSS 081007:030559+054715 (HV Ceti)
    Beardmore et al., 2012, A&A, 545, A116
• T Pyx
  • The 2011 Outburst of Recurrent Nova T Pyx: X-ray Observations Expose the White Dwarf Mass and Ejection Dynamics
    Chomiuk et al., 2014, ApJ, 788, 130
  • X-Ray Grating Observations of Recurrent Nova T Pyxidis during the 2011 Outburst
    Tofflemire et al., 2013, ApJ, 779, 22
• NSV 1436
  • Swift observations of the March 2011 outburst of the cataclysmic variable NSV 1436: a probable dwarf nova
    Osborne et al., 2011, A&A, 533, A41
• V407 Cyg
  • X-ray Emission from an Asymmetric Blast Wave and a Massive White Dwarf in the Gamma-ray Emitting Nova V407 Cyg
    Nelson et al., 2012, ApJ, 748, 43
  • The spectroscopic evolution of the symbiotic-like recurrent nova V407 Cygni during its 2010 outburst. I. The shock and its evolution
    Shore et al., 2011, A&A, 27, A98
• V598 Pup
  • X-ray and UV observations of nova V598 Puppis between 147 and 255 days after outburst
    Page et al., 2009, A&A, 507, 923
• V2491 Cyg
  • X-ray Study of Rekindled Accretion in the Classical Nova V2491 Cygni
    Takei et al., 2011, PASJ, 63, 729
  • XMM-Newton X-ray and UV observations of the fast nova V2491 Cyg during the supersoft source phase
    Ness et al., 2011, ApJ, 733, 70
  • Swift observations of the X-ray and UV evolution of V2491 Cyg (Nova Cyg 2008 No. 2)
    Page et al., 2010, MNRAS, 401, 121
  • Pre-nova X-ray observations of V2491 Cygni (Nova Cyg 2008b)
    Ibarra et al., 2009, A&A, 497, L5
• V458 Vul
  • Swift X-ray and UV monitoring of the Classical Nova V458 Vul (Nova Vul 2007)
    Ness et al., 2009, AJ, 137, 4160
• V2362 Cyg
  • Nova V2362 Cygni (nova Cygni 2006): Spitzer, Swift, and Ground-Based Spectral Evolution
    Lynch et al., 2008, AJ, 136, 1815
• V723 Cas
  • V723 CASSIOPEIA Still on in X-Rays a Bright Super Soft Source 12 Years after Outburst
    Ness et al., 2008, AJ, 135, 1328
• V5116 Sgr
  • V5116 Sagittarii, an Eclipsing Supersoft Postoutburst Nova?
    Sala, Hernanz, Ferri & Greiner, 2008, ApJ, 675, 93
• RS Oph (2006 and 2021)
  • Multi-wavelength spectroscopic study of shock-driven phenomena in explosive outbursts in symbiotic-like recurrent novae with an emphasis on RS Ophiuchi
    Azzollini et al., 2023, A&A, 674, A139
  • High-resolution X-ray spectra of RS Ophiuchi (2006 and 2021): Revealing the cause of SSS variability
    Ness et al., 2023, A&A, 670, A131
  • Fermi-LAT Gamma-ray Detection of the Recurrent Nova RS Ophiuchi during its 2021 Outburst
    Cheung et al., 2022, ApJ, 935, 44
  • Flickering Returns as RS Oph Reestablishes Quiescent Conditions Following its 2021 Nova Outburst
    Munari & Tabacco, RNAAS, 6, 103
  • The 2021 outburst of the recurrent nova RS Ophiuchi observed in X-rays by the Neil Gehrels Swift Observatory: a comparative study
    Page et al., 2022, MNRAS, 514, 1557
  • Swift Observations of the 2006 Outburst of the Recurrent Nova RS Ophiuchi. III. X-Ray Spectral Modeling
    Vaytet et al., 2011, ApJ, 740, 5
  • The Supersoft X-ray Phase of Nova RS Ophiuchi 2006
    Osborne et al., 2011, ApJ, 727, 124
  • X-Ray Spectroscopic Diagnosis of a Wind-Collimated Blast Wave and Metal-Rich Ejecta from the 2006 Explosion of RS Ophiuchi
    Drake et al., 2009, ApJ, 691, 418
  • Swift Observations of the 2006 Outburst of the Recurrent Nova RS Ophiuchi. II. One-dimensional Hydrodynamical Models of Wind-driven Shocks
    Vaytet, O'Brien & Bode, 2007, ApJ, 665, 654
  • Swift Observations of the 2006 Outburst of the Recurrent Nova RS Ophiuchi. I. Early X-Ray Emission from the Shocked Ejecta and Red Giant Wind
    Bode et al., 2006, ApJ, 652, 629
• Novae
  • Surveying the X-ray Behavior of Novae as They Emit γ-rays
    Gordon et al., 2021, ApJ, 910, 134
  • New Insights into Classical Novae
    Chomiuk, Metzger & Shen, 2021, ARA&A, 59, 391
  • The complications of learning from Super Soft Source X-ray spectra
    Ness, 2020, AdSpR, 66, 1202
  • Neil Gehrels Swift Observatory studies of supersoft novae
    Page, Beardmore & Osborne, 2020, AdSpR, 66, 1169
  • Getting to know Classical Novae with Swift
    Osborne, 2015, Journal of High Energy Astrophysics, 7, 117
  • Swift X-Ray Observations of Classical Novae. II. The Super Soft Source sample
    Schwarz et al., 2011, ApJS, 197, 31
  • Novae as a Class of Transient X-Ray Sources
    Mukai, Orio & Della Valle, 2008, ApJ, 677, 1248
  • Swift X-Ray Observations of Classical Novae
    Ness et al., 2007, ApJ, 663, 505

Swift Nova observation strategy

For Galactic Novae:

• If V_max < 5 : Observation daily, day 3 to 10 (or post X-ray peak if earlier)
• If V_max < 8 : Observation around 3 mags below maximum
• If detected :
  • If E(B-V) < 1 : monitor for SSS onset - weekly for fast novae, monthly for slow novae
    • If SSS present : monitor for SSS duration, frequency to depend on observed behaviour
  • Else : monitor monthly to end of emission
• Else : observe again in nebular phase
  • If detected : monitor monthly to end of emission

For Magellanic Cloud Novae:

• Observe MC novae with V_max < 11.5 at 6 and 9 months

All observations to be initially ~2 ks, though later observations may be longer if rapid variability or low quality spectra obtained.

This strategy has been developed as a guide rather than a fixed set of rules

Useful Links

Target of Opportunity page

Archive of Swift Nova-CV results (password-protected)