Properties of VTC J095517.5+690813 compared to other transient classes and sources assuming they are located in M81. The tabulated values are based on best-studied sources.
| Source/Type . | Radio flare timescalesa . | Peak Lum . | Radio short-term . | X-ray . | Optically . | Refe . | Candidatef . | Conflicting . | Compatible . | |
|---|---|---|---|---|---|---|---|---|---|---|
| . | (Rise) . | (Decay) . | (erg s−1 Hz−1) . | variabilityb . | detectedc . | detectedd . | . | . | propertiesg . | propertiesh . |
| . | (1) . | (2) . | (3) . | (4) . | (5) . | (6) . | . | . | . | . |
| VTC J095517.5+690813 | 2.6–112 d | >2 months | 1.5 × 1024 | N | N | N | 1 | |||
| CCSN | days–months | days–yearsi | 1026−1029 | S | S | Y | 2 | N | 3,4,5,6 | 1,2 |
| Peculiar SN (Type IIP) | days | days–yearsi | 4 × 1023−1026 | S | S | Y | 3–5 | ? | 4,5,6 | 1,2,3 |
| Magnetar giant flare | days | days–months | ≲ 1022 | N | Y | N | 6–8 | N | 3,5 | 1,2,4,6 |
| BNS merger (GW170817) | months | months–years | 2 × 1026 | N | Y | Y | 9–12 | N | 3,5,6 | 1,2,4 |
| LMXB | hours–days | days–months | ≲ 1023 | Y | Y | S | 13–25 | N | 3,4,5,6 | 1,2 |
| HMXB (Cyg X-3) | hours–days | days–months | ≲ 1024 | Y | Y | Y | 26–29 | N | 4,5,6 | 1,2,3 |
| Absorbed HMXB (SS 433) | hours–days | days | ≲ 1023 | Y | N | Y | 30–34 | N | 2,3,4,6 | 1,5 |
| IMBH (HLX-1) | days | days | 6.5 × 1026 | Y | Y | Y | 35–36 | N | 2,3,4,5,6 | 1 |
| Source/Type . | Radio flare timescalesa . | Peak Lum . | Radio short-term . | X-ray . | Optically . | Refe . | Candidatef . | Conflicting . | Compatible . | |
|---|---|---|---|---|---|---|---|---|---|---|
| . | (Rise) . | (Decay) . | (erg s−1 Hz−1) . | variabilityb . | detectedc . | detectedd . | . | . | propertiesg . | propertiesh . |
| . | (1) . | (2) . | (3) . | (4) . | (5) . | (6) . | . | . | . | . |
| VTC J095517.5+690813 | 2.6–112 d | >2 months | 1.5 × 1024 | N | N | N | 1 | |||
| CCSN | days–months | days–yearsi | 1026−1029 | S | S | Y | 2 | N | 3,4,5,6 | 1,2 |
| Peculiar SN (Type IIP) | days | days–yearsi | 4 × 1023−1026 | S | S | Y | 3–5 | ? | 4,5,6 | 1,2,3 |
| Magnetar giant flare | days | days–months | ≲ 1022 | N | Y | N | 6–8 | N | 3,5 | 1,2,4,6 |
| BNS merger (GW170817) | months | months–years | 2 × 1026 | N | Y | Y | 9–12 | N | 3,5,6 | 1,2,4 |
| LMXB | hours–days | days–months | ≲ 1023 | Y | Y | S | 13–25 | N | 3,4,5,6 | 1,2 |
| HMXB (Cyg X-3) | hours–days | days–months | ≲ 1024 | Y | Y | Y | 26–29 | N | 4,5,6 | 1,2,3 |
| Absorbed HMXB (SS 433) | hours–days | days | ≲ 1023 | Y | N | Y | 30–34 | N | 2,3,4,6 | 1,5 |
| IMBH (HLX-1) | days | days | 6.5 × 1026 | Y | Y | Y | 35–36 | N | 2,3,4,5,6 | 1 |
Notes. Some SNe go undetected in the optical band due to line-of-sight absorption.
The LMXB characteristics are based on those sources that have the brightest radio flares, including GRS 1915+105, GRO J1655-40, XTE J1748-288, H1743-322, and V404 Cyg.
The HMXB characteristics are based on Cyg X-3, which has the brightest radio flares of any accreting system in our Galaxy, and one of the few such systems that would be detectable at the distance of M81 in our VLA data.
The absorbed HMXB characteristics are based on SS 433, which is the only such system in our Galaxy.
The IMBH properties are based on HLX-1, which is the strongest IMBH candidate that also produces radio flares.
aThe typical radio flare timescales for both the rise and decay phases.
bIntrinsic short-term radio variability on timescales shorter than a day where Y = Yes, N = No, and S = Sometimes. Note that radio transients may scintillate when the source size is small.
cX-ray detection refers to an X-ray luminosity of Lx ≳ 1037 erg s−1 where Y = Yes, N = No, and S = Sometimes.
dOptical detection refers to any reported optical counterpart where Y = Yes, N = No, and S = Sometimes.
eReferences – 1: This paper, 2: Perez-Torres et al. (2015), 3: Turtle et al. (1987), 4: Pooley et al. (2002), 5: Beswick et al. (2005), 6: Frail, Kulkarni & Bloom (1999), 7: Gaensler et al. (2005), 8: Gelfand et al. (2005), 9: Hallinan et al. (2017), 10: Mooley et al. (2018a), 11: Mooley et al. (2018b), 12: Dobie et al. (2018), 13: Han & Hjellming (1992), 14: Mirabel et al. (1994), 15: Hjellming & Rupen (1995), 16: Fender et al. (1997), 17: Pooley & Fender (1997), 18: Fender et al. (1999), 19: Hjellming et al. (2000), 20: Fender & Belloni (2004), 21: Brocksopp et al. (2007), 22: McClintock et al. (2009), 23: Jonker et al. (2010), 24: Tetarenko et al. (2017), 25: Tetarenko et al. (2019), 26: Gregory & Kronberg (1972), 27: Waltman et al. (1995), 28: Miller-Jones et al. (2004), 29: Corbel et al. (2012), 30: Fiedler et al. (1987), 31: Trushkin, Goranskij & Kotani (2006), 32: Trushkin, Nizhelskij & Zhekanis (2011), 33: Trushkin, Nizhelskij & Tsybulev (2012), 34: Trushkin et al. (2018), 35: Webb et al. (2012), 36: Cseh et al. (2015a).
fCandidate refers to whether the corresponding source type is a viable classification for VTC J095517.5+690813 where N = No and ? = possible.
gCharacteristics that are not consistent with VTC J095517.5+690813. The listed numbers correspond to the number labelling of the columns.
hCharacteristics that are consistent with VTC J095517.5+690813. The listed numbers correspond to the number labelling of the columns.
iRadio flare decay timescales of years mainly pertain to interacting SNe (see Section 4.2.1).
Properties of VTC J095517.5+690813 compared to other transient classes and sources assuming they are located in M81. The tabulated values are based on best-studied sources.
| Source/Type . | Radio flare timescalesa . | Peak Lum . | Radio short-term . | X-ray . | Optically . | Refe . | Candidatef . | Conflicting . | Compatible . | |
|---|---|---|---|---|---|---|---|---|---|---|
| . | (Rise) . | (Decay) . | (erg s−1 Hz−1) . | variabilityb . | detectedc . | detectedd . | . | . | propertiesg . | propertiesh . |
| . | (1) . | (2) . | (3) . | (4) . | (5) . | (6) . | . | . | . | . |
| VTC J095517.5+690813 | 2.6–112 d | >2 months | 1.5 × 1024 | N | N | N | 1 | |||
| CCSN | days–months | days–yearsi | 1026−1029 | S | S | Y | 2 | N | 3,4,5,6 | 1,2 |
| Peculiar SN (Type IIP) | days | days–yearsi | 4 × 1023−1026 | S | S | Y | 3–5 | ? | 4,5,6 | 1,2,3 |
| Magnetar giant flare | days | days–months | ≲ 1022 | N | Y | N | 6–8 | N | 3,5 | 1,2,4,6 |
| BNS merger (GW170817) | months | months–years | 2 × 1026 | N | Y | Y | 9–12 | N | 3,5,6 | 1,2,4 |
| LMXB | hours–days | days–months | ≲ 1023 | Y | Y | S | 13–25 | N | 3,4,5,6 | 1,2 |
| HMXB (Cyg X-3) | hours–days | days–months | ≲ 1024 | Y | Y | Y | 26–29 | N | 4,5,6 | 1,2,3 |
| Absorbed HMXB (SS 433) | hours–days | days | ≲ 1023 | Y | N | Y | 30–34 | N | 2,3,4,6 | 1,5 |
| IMBH (HLX-1) | days | days | 6.5 × 1026 | Y | Y | Y | 35–36 | N | 2,3,4,5,6 | 1 |
| Source/Type . | Radio flare timescalesa . | Peak Lum . | Radio short-term . | X-ray . | Optically . | Refe . | Candidatef . | Conflicting . | Compatible . | |
|---|---|---|---|---|---|---|---|---|---|---|
| . | (Rise) . | (Decay) . | (erg s−1 Hz−1) . | variabilityb . | detectedc . | detectedd . | . | . | propertiesg . | propertiesh . |
| . | (1) . | (2) . | (3) . | (4) . | (5) . | (6) . | . | . | . | . |
| VTC J095517.5+690813 | 2.6–112 d | >2 months | 1.5 × 1024 | N | N | N | 1 | |||
| CCSN | days–months | days–yearsi | 1026−1029 | S | S | Y | 2 | N | 3,4,5,6 | 1,2 |
| Peculiar SN (Type IIP) | days | days–yearsi | 4 × 1023−1026 | S | S | Y | 3–5 | ? | 4,5,6 | 1,2,3 |
| Magnetar giant flare | days | days–months | ≲ 1022 | N | Y | N | 6–8 | N | 3,5 | 1,2,4,6 |
| BNS merger (GW170817) | months | months–years | 2 × 1026 | N | Y | Y | 9–12 | N | 3,5,6 | 1,2,4 |
| LMXB | hours–days | days–months | ≲ 1023 | Y | Y | S | 13–25 | N | 3,4,5,6 | 1,2 |
| HMXB (Cyg X-3) | hours–days | days–months | ≲ 1024 | Y | Y | Y | 26–29 | N | 4,5,6 | 1,2,3 |
| Absorbed HMXB (SS 433) | hours–days | days | ≲ 1023 | Y | N | Y | 30–34 | N | 2,3,4,6 | 1,5 |
| IMBH (HLX-1) | days | days | 6.5 × 1026 | Y | Y | Y | 35–36 | N | 2,3,4,5,6 | 1 |
Notes. Some SNe go undetected in the optical band due to line-of-sight absorption.
The LMXB characteristics are based on those sources that have the brightest radio flares, including GRS 1915+105, GRO J1655-40, XTE J1748-288, H1743-322, and V404 Cyg.
The HMXB characteristics are based on Cyg X-3, which has the brightest radio flares of any accreting system in our Galaxy, and one of the few such systems that would be detectable at the distance of M81 in our VLA data.
The absorbed HMXB characteristics are based on SS 433, which is the only such system in our Galaxy.
The IMBH properties are based on HLX-1, which is the strongest IMBH candidate that also produces radio flares.
aThe typical radio flare timescales for both the rise and decay phases.
bIntrinsic short-term radio variability on timescales shorter than a day where Y = Yes, N = No, and S = Sometimes. Note that radio transients may scintillate when the source size is small.
cX-ray detection refers to an X-ray luminosity of Lx ≳ 1037 erg s−1 where Y = Yes, N = No, and S = Sometimes.
dOptical detection refers to any reported optical counterpart where Y = Yes, N = No, and S = Sometimes.
eReferences – 1: This paper, 2: Perez-Torres et al. (2015), 3: Turtle et al. (1987), 4: Pooley et al. (2002), 5: Beswick et al. (2005), 6: Frail, Kulkarni & Bloom (1999), 7: Gaensler et al. (2005), 8: Gelfand et al. (2005), 9: Hallinan et al. (2017), 10: Mooley et al. (2018a), 11: Mooley et al. (2018b), 12: Dobie et al. (2018), 13: Han & Hjellming (1992), 14: Mirabel et al. (1994), 15: Hjellming & Rupen (1995), 16: Fender et al. (1997), 17: Pooley & Fender (1997), 18: Fender et al. (1999), 19: Hjellming et al. (2000), 20: Fender & Belloni (2004), 21: Brocksopp et al. (2007), 22: McClintock et al. (2009), 23: Jonker et al. (2010), 24: Tetarenko et al. (2017), 25: Tetarenko et al. (2019), 26: Gregory & Kronberg (1972), 27: Waltman et al. (1995), 28: Miller-Jones et al. (2004), 29: Corbel et al. (2012), 30: Fiedler et al. (1987), 31: Trushkin, Goranskij & Kotani (2006), 32: Trushkin, Nizhelskij & Zhekanis (2011), 33: Trushkin, Nizhelskij & Tsybulev (2012), 34: Trushkin et al. (2018), 35: Webb et al. (2012), 36: Cseh et al. (2015a).
fCandidate refers to whether the corresponding source type is a viable classification for VTC J095517.5+690813 where N = No and ? = possible.
gCharacteristics that are not consistent with VTC J095517.5+690813. The listed numbers correspond to the number labelling of the columns.
hCharacteristics that are consistent with VTC J095517.5+690813. The listed numbers correspond to the number labelling of the columns.
iRadio flare decay timescales of years mainly pertain to interacting SNe (see Section 4.2.1).
This PDF is available to Subscribers Only
View Article Abstract & Purchase OptionsFor full access to this pdf, sign in to an existing account, or purchase an annual subscription.
