Issue |
A&A
Volume 499, Number 3, June I 2009
|
|
---|---|---|
Page(s) | 649 - 652 | |
Section | Astrophysical processes | |
DOI | https://doi.org/10.1051/0004-6361/200912034 | |
Published online | 08 April 2009 |
23 GHz VLBI observations of SN 2008ax
(Research Note)
I. Martí-Vidal1,2 - J. M. Marcaide1 - A. Alberdi3 - J. C. Guirado1 - M. A. Pérez-Torres3 - E. Ros2,1 - I. I. Shapiro4 - R. J. Beswick5 - T. W. B. Muxlow5 - A. Pedlar5 - M. K. Argo6 - S. Immler7 - N. Panagia8,9,10 - C. J. Stockdale11 - R. A. Sramek12 - S. Van Dyk13 - K. W. Weiler14
1 - Dpt. Astronomia i Astrofísica, Universitat de València,
C/ Dr. Moliner 50, 46100 Burjassot, Spain
2 -
Max-Planck-Institut für Radioastronomie,
Auf dem Hügel 69, 53121 Bonn, Germany
3 -
Instituto de Astrofísica de Andalucía (CSIC),
C/ Camino bajo de Huétor 50, 18008 Granada, Spain
4 -
Harvard-Smithsonian Center for Astrophysics,
60 Garden St., MS 51, Cambridge, MA 02138, USA
5 -
Jodrell Bank Observatory,
Macclesfield, Cheshire SK11 9DL, UK
6 -
Department of Imaging and Applied Physics,
Curtin University of Technology,
Bentley, WA 6845, Australia
7 -
NASA Goddard Space Flight Center,
Astrophysics Science Division, Code 662, Greenbelt, MD 20771, USA
8 -
Space Telescope Science Institute, 3700 San Martin Drive,
Baltimore, Maryland 21218, USA
9 -
INAF - Osservatorio Astrofisico di Catania,
via S. Sofia 78, 95123, Catania, Italy
10 -
Supernova Ltd, OYV #131, Northsouth Rd.,
Virgin Gorda, British Virgin Islands
11 -
Department of Physics, Marquette University,
PO Box 1881, Milwaukee, WI 53201-1881, USA
12 -
National Radio Astronomy Observatory,
PO Box O, Socorro, NM 87801, USA
13 -
University of California, Astronomy Department,
Berkeley, California 94720, USA
14 -
Naval Research Laboratory,
Code 7210, Washington, DC 20375-5320, USA
Received 10 March 2009 / Accepted 24 March 2009
Abstract
We report on phase-referenced 23 GHz Very-Long-Baseline-Interferometry (VLBI) observations
of the type IIb supernova SN 2008ax, made with the Very Long Baseline Array (VLBA) on 2 April
2008 (33 days after explosion). These observations resulted in a
marginal detection of the supernova. The total flux density recovered from our VLBI image is
mJy (one standard deviation). As it appears, the structure may be interpreted as
either a core-jet or a double source. However, the supernova structure could be somewhat confused
with a possible close by noise peak. In such a case, the recovered flux density would decrease to
mJy, compatible with the flux densities measured with the VLA at
epochs close in time to our VLBI observations. The lowest
average expansion velocities derived from our observations are
km s-1
(case of a double source) and
km s-1 (taking the weaker
source component as a spurious, close by, noise peak, which is the more likely interpretation).
These velocities are 7.3 and 2 times higher, respectively, than the maximum ejecta velocity
inferred from optical-line observations.
Key words: galaxies: individual: NGC 4490 - radio continuum: stars - supernovae: individual: SN 2008ax - supernovae: general
1 Introduction
Supernova SN 2008ax was discovered in galaxy NGC 4490 on 3
March 2008 (Mostardi et al. 2008) at the position
and
.
The host galaxy is
8 Mpc distant (de Vaucouleurs
1976; we assume an uncertainty of 1 Mpc for the distance),
and is dynamically interacting with NGC 4485
(forming the pair Arp 269). Likely as a consequence of this
interaction, NGC 4490 has a relatively high star formation rate
(Viallefond et al. 1980), which should
results in a correspondingly high supernova rate.
We assume the discovery date of the supernova was the same as the explosion date, since 6 h before its discovery, the location of the supernova was imaged with a limiting magnitude of 18.3 and no emission was detected (Nakano 2008). Radio emission from SN 2008ax was monitored with the VLA beginning on 3 March 2008, shortly after its discovery (see Stockdale et al. 2008a,b), with positive detections made at 4.9, 8.4, and 22.5 GHz, beginning on 7 March 2008. These detections were all in the millijansky range. The early part of the radio light curve of this supernova is qualitatively similar to that of SN 1993J. Since supernova SN 2008ax was also cataloged as type IIb (Chornock 2008), as was SN 1993J, there was evidence to believe that the radio emission of SN 2008ax would continue its evolution in a similar way to SN 1993J's. In such a case, the flux density of SN 2008ax should have risen well above the VLBI detectability limit near the end of March 2008.
On 11 March 2008, we proposed a target-of-opportunity set of global VLBI observations of SN 2008ax at 23 GHz, in order to detect the supernova radio structure and, possibly, its expansion. Only antennas of the VLBA were allocated and only on 2 April 2008. Unfortunately, the flux density started to drop faster than expected by that time, resulting in a marginal detection of the supernova. In the next section we describe the details of our VLBI observations, and in Sect. 3 we present our results and conclusions.
2 Observations and data reduction
We observed supernova 2008ax on 2 April 2008, with the VLBA (10 identical 25 m diameter antennas spread over the USA from the Virgin Islands to Hawaii). The recording rate was set to 256 Mbps, with 2-bit sampling and single polarization mode (LCP), covering a total bandwidth of 64 MHz (8 baseband channels, of 8 MHz width each). Our observations were cross-correlated at the Array Operations Center of the National Radio Astronomy Observatory (NRAO) in Socorro (New Mexico, USA), using an averaging time of 2 s.
The observations of SN 2008ax were made in phase-reference mode. Each scan of
the supernova was of 2 min duration, and short observations (
40 s)
of strong, close by sources were interleaved between these scans of the supernova.
Since the 23 GHz flux densities of these close by radio sources
were unknown at the time of the observations, we chose the two closest, which were also
the strongest at 15 GHz. Each pass of the
recording tapes (22 min long) was then assigned to one of these two calibrators in
an alternating scheme. The 12-h long set of observations could, thus, be
divided into two sets of roughly equal size. In the first one, we observed the supernova
using the source J1224+4335 as the phase calibrator (located 2.23 degrees from the
supernova) and in the second one we used the source J1225+3914 as the phase
calibrator (located 2.57 degrees from the supernova).
After the cross correlation, the data were imported into the NRAO Astronomical Image Processing System ( AIPS) for calibration. We performed the amplitude calibration using gain curves and system temperatures measured at all antennas. We then used in the scans of the supernova the time-interpolated antenna gains obtained from hybrid mapping of the calibrators. The phase calibration (with account taken of the structures of the calibrators) was performed with standard phase-reference calibration techniques. The data were then exported for further reduction in DIFMAP (Shepherd et al. 1995).
3 Results and conclusions
The flux density of the calibrator source J1224+4335, obtained from hybrid mapping,
is mJy and the flux density of the other calibrator source, J1225+3914,
obtained with the same procedure, is
mJy. Uncertainties are 3 times the
root-mean-square, rms, of the hybrid-map residuals (see Readhead & Wilkinson 1978).
There is no clear detection of SN 2008ax in any of the phase-referenced images obtained
using both calibrators. There is not even a clear flux density peak in the
images obtained from the totality of supernova visibilities (i.e., dynamic range above
6),
regardless of the sky coverage of the image or the
weighting scheme applied in Fourier space. However, when the phase-reference
calibrator J1224+4335 (i.e., the strongest and closest calibrator) is used,
there is a possible detection of the supernova. The detection arises from applying
a visibility weighting in Fourier space with the weight of a pixel proportional to the
square of the signal-to-noise ratio (SNR) of the visibilities inside that pixel (i.e.,
we increase the array sensitivity in the Fourier inversion). We additionally taper the
visibilities using a Gaussian, centered at the origin of the uv-plane, with a Full Width at
Half Maximum (FWHM) of 500 M
.
The image obtained with such a visibility weighting
has a peak flux density located at 0.08 mas to the West and 9.2 mas to the South of
the position used at the correlator, which was taken from X-band VLA observations made
on 8 March 2009. Therefore, the peak flux density detected is located at
and
,
with an
uncertainty of 0.05 mas, which is the size of the interferometric beam divided by
2 times the dynamic range of the image (Thomson et al. 1986).
Since this position is based on a phase-reference to J1224+4335 at 23 GHz, we notice
that opacity effects in the jet of this source (see Fig. 1) could
introduce a systematic shift of several
mas in the supernova position (the correlation position of J1224+4335 was taken from the
VLBA Calibrator Survey at 8.4 GHz; see Beasley et al. 2002).
Decreasing the FWHM of the Gaussian taper, or weighting each pixel with a higher power of
the visibility SNR, results in a slightly better detection of the supernova but, due to
the large decrease in resolution, at the price of a detailed detection of radio structure.
![]() |
Figure 1: Hybrid image of source J1224+4335 obtained from our observations. The FWHM of the convolving CLEAN beam is shown at the bottom-left corner. |
Open with DEXTER |
![]() |
Figure 2: CLEAN phase-referenced image of SN 2008ax (see text). The FWHM of the convolving beam is shown at the bottom-left corner. |
Open with DEXTER |
![]() |
Figure 3:
Dirty image of SN 2008ax with a sky coverage of
|
Open with DEXTER |
After performing a CLEAN deconvolution in the region of the flux density peak, we
obtain the image shown in Fig. 2. The rms of the residuals is
0.087 mJy beam-1 and the peak flux density is 0.395 mJy beam-1, so the
dynamic range of the image is 4.7. The total flux density obtained after a
deconvolution using the CLEAN algorithm is 0.8 mJy. Remarkably,
the flux density recovered from our VLBI image is a factor 1.7 larger than the flux
densities registered with the VLA by Stockdale et al. (2008b) at epochs close in
time to the epoch of our observations (
mJy on April 1, and
mJy on April 3).
This large discrepancy indicates that the source structure shown
in Fig. 2 may be a chance superposition of a marginal detection (North) and
a prominent noise peak (South), as we explain below.
The integrated flux density of each of the noise peaks of the residual image in a
mas square around the source is less than 0.4 mJy (i.e., less than 50%
of the integrated flux density of the source). We show this wide-field image in
Fig. 3.
If the structure shown in Fig. 2 is real, does it correspond to a core-jet or is it part of a shell? Or, as we suggest above, can this structure be a combination of a marginal detection (North) with a stronger noise peak (South) than elsewhere in the map? Difficult to say.
Case 1. Partial shell-like structure
For the radio structure part of a shell, we can compare its 50% contour
level with that of a shell model convolved with the same beam. For a shell model with
a fractional shell width of 0.3, which is the shell width found for SN 1993J by
Marcaide et al. (2009), the outer radius of SN 2008ax
would be
mas (hereafter, all the uncertainties given are equal to the
square root of the corresponding diagonal element of the covariance matrix, with the
errors having been first uniformly scaled so that the reduced
is equal to 1). This size translates into an average expansion velocity of
km s-1, which is superluminal. Indeed, we still obtain
superluminal expansion velocities if we change the fractional shell width to different,
unrealistic, values such as 0.1 (a narrower shell width translates into a smaller fitted shell
size). Hence, it is unlikely that the radio structure is part of an expanding shell.
Case 2. Double source
If we instead fit the visibilities to two point sources, one to model the brightness peak
(at the North) and the other one to model the source extension towards the South, we find
components of
and
mJy, separated by
mas. This result translates into an average relative velocity between components of
km s-1, which is
superluminal. If
the two components were moving in opposite directions with respect to the explosion
center, the average expansion velocity of the radiostructure would be
km s-1, a factor
7.3 higher than the maximum ejecta
velocity estimated from the optical-line emission of this supernova
(
km s-1, Blondin 2008). This velocity is also much
higher than the typical expansion velocities of the radiostructures of other supernovae
(
km s-1). Hence, the two-point source model is also unlikely.
Case 3. Detection with a close by noise peak
Perhaps, then, we could consider that the structure shown in the map is due to a chance (near)
superposition of a marginally detected radio source and a noise peak. In this case, the
radio emission would not be resolved and its detection would be even more marginal. Fitting
a shell model (with a fractional width of 0.3) to the northern flux density peak results in a
source outer diameter of
mas and
a flux density of
mJy. We notice that this flux density is consistent with
the flux densities registered by Stockdale et al. (2008b) at the same radio
frequency and at epochs enclosing that of our VLBI
observations. The resulting average expansion velocity is
km s-1, a factor of 2 larger than the velocity inferred from optical-line emission. This velocity is
also
3 times larger than the expansion velocities of the other radio
supernovae that were observed with VLBI (<
km s-1), and would imply
(if we assume a non-decelerated expansion at least until the epoch of our observations) a
fractional width of the shocked
circumstellar region of
0.5. To obtain this estimate, we assume that the optical-line
emission comes from a region close to the inner edge of the shocked ejecta (see Chevalier &
Fransson 1994). This fractional width is much larger than that found for
SN 1993J and those predicted from different models of type II supernovae (Chevalier
1982). Considering a decelerated supernova expansion would result in
even larger fractional-shell width estimates.
General remarks
In short, every model used in our analysis results in a supernova size
much larger than expected from the optical-line velocities of this supernova
and the expansion velocities found for all supernovae that could be
imaged with VLBI. The lowest average expansion velocity compatible with our VLBI data is a factor
of 2 larger than the velocity inferred from optical-line emission. However, despite the apparent
significance of our measurements (4
for the
flux density and 5
for the size), we have obtained only a marginal
detection of SN 2008ax with our VLBI observations.
Acknowledgements
The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. This work has been partially funded bygrants AYA2006-14986-CO2-01 and AYA2006-14986-C02-02 of the Spanish DGICYT. K.W.W. thanks the Office of Naval Research for the 6.1 funding supporting this research. I.M.V. is a fellow of the Alexander von Humboldt Foundation.
References
- Beasley, A. J., Gordon, D., Peck, et al. 2002, ApJ, 141, 13 [NASA ADS] [CrossRef] (In the text)
- Blondin, S., Filippenko, A. V., Foley, R. J., et al. 2008, CBET, 1285, 1 [NASA ADS] (In the text)
- Chevalier, R. A. 1982, ApJ, 258, 790 [NASA ADS] [CrossRef] (In the text)
- Chevalier, R. A., & Fransson, C. 1994, ApJ, 420, 268 [NASA ADS] [CrossRef] (In the text)
- Chornock, R., Filippenko, A. V., Li, W., et al. 2008, CBET, 1298, 1 [NASA ADS] (In the text)
- Marcaide, J. M., Martí-Vidal, I., Alberdi, A., et al. 2009, ApJ, submitted (In the text)
- Mostardi, R., Li, W., & Filippenko, A. V. 2008, CBET, 1280, 1 [NASA ADS] (In the text)
- Nakano, S. 2008, CBET, 1286, 1 [NASA ADS] (In the text)
- Thomson, A. R., Moran, J. M., & Swenson, G. W. 1986, Interferometry and Synthesis in Radio Astronomy (New York: Wiley) (In the text)
- Readhead, A. C. S., & Wilkinson, P. N. 1978, ApJ, 223, 25 [NASA ADS] [CrossRef] (In the text)
- Shepherd M. C., Pearson T. J., & Taylor G. B. 1995, BAAS, 26, 987 [NASA ADS] (In the text)
- Stockdale, C. J., Weiler, K. W., Immler, S., et al. 2008a, CBET, 1299, 1 [NASA ADS] (In the text)
- Stockdale, C. J., Weiler, K. W., Immler, S., et al. 2008b, ATEL, 1439, 1 [NASA ADS] (In the text)
- de Vaucouleurs, G., de Vaucouleurs, A., & Corwin, J. R. 1976, Second reference catalogue of bright galaxies (Austin: University of Texas Press) (In the text)
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All Figures
![]() |
Figure 1: Hybrid image of source J1224+4335 obtained from our observations. The FWHM of the convolving CLEAN beam is shown at the bottom-left corner. |
Open with DEXTER | |
In the text |
![]() |
Figure 2: CLEAN phase-referenced image of SN 2008ax (see text). The FWHM of the convolving beam is shown at the bottom-left corner. |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Dirty image of SN 2008ax with a sky coverage of
|
Open with DEXTER | |
In the text |
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