Optical and Near‐Infrared Photometry of the Type Ia Supernova 2000E in NGC 6951

Valentini, G.; Carlo, E. Di; Massi, F.; Dolci, M.; Arkharov, A. A.; Larionov, V. M.; Pastorello, A.; Paola, Andrea; Benetti, S.; Cappellaro, E.; Turatto, M.; Pedichini, Fernando; D’Alessio, F.; Garatti, A. Caratti o; Causi, G. Li; Speziali, R.; Danziger, I. J.; Tornambé, Amedeo

doi:10.1086/377448

Cited by 62 publications

(42 citation statements)

References 51 publications

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“…This behavior in the NIR colors during the rebrightening is not only totally at odds with that of other nonstellar objects, like SNe Ia (e.g., Valentini et al 2003), where dust is expected to play quite a marginal role in the light emission, but also different from, e.g., that of a ''dusty'' CC SN like the Type IIn SN 1999el (Di Carlo et al 2002). In the latter case, dust is expected to be the main cause of the observed NIR excess, and, in fact, the NIR colors evolve below the reddening band of the stellar main sequence in an (H À K) versus (J À H) diagram.…”

Section: Nir Color Evolutionmentioning

confidence: 68%

“…Unfortunately, good NIR light curves ( LCs) spanning until late epochs are available only in a few cases. The observatories of Teramo ( Italy), Rome ( Italy), and Pulkovo (Russia) are involved in a program aimed at providing accurate LCs of SNe in the NIR (Di Carlo et al 2002;Di Paola et al 2002;Valentini et al 2003) by using a dedicated 1 m class telescope equipped with a NIR camera. In the framework of this program, we present the results of our NIR follow-up of SN 2006jc, discovered on 2006 October 9.752 UT (Nakano et al 2006) in the galaxy UGC 4904.…”

Section: Introductionmentioning

confidence: 99%

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Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

Carlo

Corsi

Arkharov

et al. 2008

Astrophysical Journal

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In the framework of a program for the monitoring of supernovae in the near-infrared (NIR) carried out by the Teramo, Rome, and Pulkovo observatories with the AZT-24 telescope, we observed the supernova SN 2006jc in the J, H, and K photometric bands during a period of 7 months, starting $36 days after its discovery. Our observations evidence a NIR rebrightening, peaking $70 days after discovery, along with a reddening of (H À K) and (J À H) colors until 120 days after discovery. After that date, (J À H) seems to evolve toward bluer colors. Our data, complemented with IR and optical observations found in the literature, show that the rebrightening is produced by hot, newly formed dust surrounding the supernova.

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Section: Nir Color Evolutionmentioning

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

Carlo

Corsi

Arkharov

et al. 2008

Astrophysical Journal

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“…The resulting zeropoints are listed in Table 13 along with the tabulated flux for a zero-magnitude star and the effective wavelengths of the employed photometric system. Thus, we determine the bolometric luminosity as the area of trapezium connecting the BVRIJHK points (Valentini et al 2003), and we assume the average distance modulus derived in this work. To correct the bolometric LC for missing data in the U passband, we set the flux to zero at 3000 Å and extrapolate the flux at 3600 Å (see Suntzeff 1996).…”

Section: Bolometric Behaviour Of Sn 2008fvmentioning

confidence: 99%

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Biscardi

Brocato

Arkharov

et al. 2012

A&A

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Aims. We present optical and near-infrared (NIR) photometry of supernova (SN) 2008fv and a brief investigation of SN type Ia to search for possible correlations between the properties of NIR light curves and the optical decline rate. Methods. We analyse our BVRI and JHK observations to derive light curves (LCs), colour curves, and the bolometric behaviour of SN 2008fv. Data range from about five days before to two months after maximum. We also collect a database of the main characteristics of NIR LCs of SNe Ia available in literature. Results. We find close similarities between the observed LCs of the SN event studied here and SN 2000E. SN 2008fv is a slow-declining SNe Ia with a post-maximum decline of Δm 15,B = 0.96 ± 0.08 mag and a B-band maximum luminosity of M B,0 = −19.40 ± 0.1 mag, close to the value of normal SNe Ia. The optical and NIR data allow us to constrain the host galaxy reddening of NGC 3147, E(B−V) = 0.22 ± 0.05 mag and its distance μ = 33.2 ± 0.1 mag. Furthermore, we derive a synthesized 56 Ni mass of about 0.7 M , by using the well-known relation between the maximum luminosity of the uvoir bolometric light curve and the initial content of 56 Ni. We investigate the correlation between the NIR characteristics of LCs and optical properties by collecting data of a sample of 40 SNe. We derive quantitative relationships involving the epoch of the secondary maximum in the JHK bands and the decline rate Δm 15 (B). Further, we find no correlations between Δm 15 measured in the JHK bands and the optical Δm 15 (B). In contrast, quite evident correlations with the Δm 15 (B) and Δm 40 (J)/Δm 15 (H).

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“…Therefore, exactly how the group boundaries were drawn was not important. (Gerardy et al 2004), and SN 2004S (Krisciunas et al 2007); the broad-line SN 1983G (McCall et al 1984 and SN 2002er (Kotak et al 2006); and the shallow-silicon SN 1999aa , SN 1999ac (Garavini et al 2005), SN 2000E (Valentini et al 2003), SN 2005cg (Quimby et al 2006), and SN 2003fg (the proposed super-Chandrasekhar SN Ia, also known as SNLS-03D3bb; Howell et al 2006;Jeffery et al 2007a; but see also Hillebrandt et al 2007). SN 1999ac is a borderline case: in Figure 1, it falls between two core-normals, but on the basis of the shape, depth, and width of the 6100 Å absorption, we include it with the shallow-silicons.…”

Section: Introductionmentioning

confidence: 99%

Comparative Direct Analysis of Type Ia Supernova Spectra. III. Premaximum

Branch¹,

Troxel²,

Jeffery³

et al. 2007

PUBL ASTRON SOC PAC

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ABSTRACT.A comparative study of spectra of 21 Type Ia supernovae (SNe Ia) obtained about 1 week before maximum light, and 8 spectra obtained 11 or more days before maximum, is presented. To a large extent, the premaximum spectra exhibit the defining characteristics of the four groups defined in Paper II (core normal, broad line, cool, and shallow silicon). Comparisons with SYNOW synthetic spectra show that all strong features and most weak ones can be accounted for in a plausible way. The issues of detached high-velocity features, the possible ubiquity of carbon clumps, the maximum detectable ejecta velocities, and the possibility of blueshifted emission-line peaks are discussed.

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Optical and Near‐Infrared Photometry of the Type Ia Supernova 2000E in NGC 6951

Cited by 62 publications

References 51 publications

Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Comparative Direct Analysis of Type Ia Supernova Spectra. III. Premaximum

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