Simulations and interpretation of the 6 cm MERLIN images of the classical nova V723 Cas

Simulations and interpretation of the 6-cm MERLIN images of the classical nova V723 Cas

Abstract

We compare the predictions of simple models for the radio emission from classical novae with the MERLIN radio observations of nova V723 Cas (Nova Cas 1995). Spherically symmetric and ellipsoidal radiative transfer models are implemented in order to generate synthetic emission maps. These are then convolved with an accurate representation of the coverage of MERLIN. The parameters and geometry of the shell model are based on those returned by fitting models to the observed light curve. This allows direct comparison of the model images with the nine 6 cm MERLIN images of V723 Cas.

It is found that the seemingly complex structure (clumping, apparent rotation) evident in the observations can actually be reproduced with a simple spherical emission model. The simulations show that a 24 hour track greatly reduces the instrumental effects and the synthetic radio map is a closer representation of the true (model) sky brightness distribution. It is clear that interferometric arrays with sparse coverage (e.g. MERLIN, VLBA) will be more prone to these instrumental effects especially when imaging ring-like objects with time dependent structure variations. A modelling approach such as that adopted here is essential when interpreting observations.

keywords:
stars: novae, cataclysmic variables – stars: novae: individual (V723 Cas) – radio continuum: stars – techniques: interferometric
12

1 Introduction

Classical novae are the result of thermonuclear explosions in interacting binary stars. The system consists of a hot white dwarf primary with a main sequence secondary companion. The secondary is thought to fill its Roche lobe and transfers hydrogen-rich material via an accretion disc onto the surface of the white dwarf. When the pressure in the degenerate material at the base of the accreted layer reaches a critical value a thermonuclear runaway takes place (Starrfield 1989), ejecting 10–10 M of material into the interstellar medium at velocities of up to several thousand kilometres per second. This causes an increase in the bolometric luminosity of the system of a few orders of magnitude over a timescale of a few days.

Radio emission from the nova starts to develop at a later time than the optical. The white dwarf star photoionises the ejecta giving rise to free-free emission at temperatures of approximately 10 K. The evolution of the ejecta is generally rapid, allowing radio interferometric observations to track the expanding shell as it brightens and then fades over favourable timescales (e.g. Taylor et al, 1987; Eyres et al, 1996, 2000, 2005; Heywood et al, 2002, 2005). Both radio and optical images of classical novae often show non-homogeneous, albeit spherical or ellipsoidal structures. A feature common to all MERLIN observations of novae is apparent rotation between epochs.

In this paper we investigate the structure seen in MERLIN observations of V723 Cas (Nova Cas 1995) using models fitted to the radio light curve (Heywood et al 2005 - hereafter Paper I). The simulations presented in this paper provide an insight into how the radio images that result from interferometer observations relate to the true distribution of the emitting material. Radio images are often cited during discussions of the morphology of nova shells. Although it is common knowledge that interferometer images are an approximation of the true sky brightness distribution, it has not previously been determined just how many of the features which are common to radio observations of novae are due to the interferometer and the aperture synthesis process. The goal for this investigation is to generate synthetic emission maps based on shell models to be subsequently convolved with an accurate coverage model of the MERLIN interferometer.

Descriptions of the shell models used are presented in Section 2. A radiative transfer solution is implemented for both a spherically symmetric and an ellipsoidal shell based on the models described in Paper I. This process results in simulated emission maps which are then convolved with a model. In all cases this process, described in Section 3, is consistent with the genuine MERLIN observations of V723 Cas presented in Paper I and reproduced in Figure 1. This facilitates direct comparisons between the real and simulated radio images.

\begin{picture}(10.0,21.0)\put(-4.0,2.2){\special{psfile=merlin.eps vscale=80 % hscale=80 voffset=1 hoffset=0}} \end{picture}
Figure 1: 6 cm MERLIN images of the nova V723 Cas, as published by Heywood et al. (2005), reproduced here for comparison with the simulations. The contour levels are (-3, 3, 3, 6, 6, 12, 12…) 0.15 mJy.

2 Simulations

Model images of the sky brightness distribution are generated by solving the line of sight equations of radiative transfer through a model emitting region. Descriptions of the radiative transfer code and the model shell geometries are presented in this section, together with images showing the predicted brightness distributions. Synthetic interferometer maps are derived by masking the Fourier transform of these images with the coverage of the interferometer and then inverting the transform, this process is described in Section 3.

2.1 Axisymmetric radiative transfer

The radiative transfer code uses cylindrical polar coordinates to define the emitting region as used by, for example, Dougherty et al (2003). The coordinate system is shown in Figure 2. The shell model is constructed by creating a density function in the plane defined by and . A 3D shell is created by mirroring the distribution about the plane defined by and and rotating through 360 degrees about the axis. Thus the quarter circles indicated by the solid lines in Figure 2 would define full spherical regions. The configuration shown in Figure 2 is representative of the Hubble flow model described in Paper I (and previously by Seaquist & Palimaka, 1977, and by Hjellming et al, 1979) and is discussed further below.

The density and temperature are defined in an array of dimensions 256 512 in and respectively and when the coordinate transform is applied to define the 3D emitting region the result is mapped on to a 256 256 pixel image. The arrays defining the image are chosen to be 2 in size, where is an integer, so that the Fast Fourier Transform (FFT) technique can be applied when convolving these images in the plane.

The frequency of the radiation is specified and the radiative transfer equations are solved along gridded lines of sight through the shell. The code then calls a Hierarchical Data System (HDS) library which outputs images of intensity, optical depth and brightness temperature in the STARLINK N-dimensional Data Format (NDF).

Figure 2: Coordinate system for the axisymmetric radiative transfer code. This figure shows how the shell is defined in the cylindrical polar coordinates used by the model.

An inclination angle for the orientation of the model can also be specified. This is denoted by and is the angle between the axis in the plane of the sky and the axis of the coordinate system.

2.2 Spherically symmetric Hubble flow model

The Hubble flow model applied to V723 Cas in Paper I is used as the basis for the first run of the axisymmetric radiative transfer code. The values of mass and inner and outer ejection velocity returned by the best fit routine are used to define the density and the shell geometry for this model. The inner and outer shell boundaries, and consequently the shell density, are time dependent and emission maps are created with epochs corresponding to the 6 cm MERLIN observations presented in Paper I.

The density function of the Hubble flow model is given by

(1)

which is a function of , the radial distance from the centre of the shell, and also of and , the radii of the inner and outer shell boundaries respectively. Hence when the shell is defined in the radiative transfer code the density array is filled according to

(2)

for . This is a function of and and the parameters and which are fixed for a given epoch. Similarly for the temperature is fixed at 17000 K (see Paper I). Outside the shell boundaries the density is assumed to be zero and the temperature is set at 100 K. The inclination angle is a redundant parameter in the spherical case.

The nine model intensity maps created by this process are presented in Figure 3 where it can be seen how initially the emission is entirely optically thick. As the material expands the outer layers start to become optically thin and eventually the inner boundary of the shell is revealed as a bright ring.

\begin{picture}(10.0,21.0)\put(-3.9,2.8){\special{psfile=sph_no_uv_bw.eps % vscale=80 hscale=80 voffset=1 hoffset=0}} \end{picture}
Figure 3: Model intensity distributions for the Hubble flow model. These maps are calculated at times following outburst shown in each panel, coinciding with the 6 cm MERLIN observations of V723 Cas. The greyscale is in units of mJy.

2.3 Ellipsoidal shell model

Some observations of classical novae show prolate ellipsoidal shells (e.g. FH Ser, Gill & O’Brien, 2000) and the intention here is to determine whether it is possible to distinguish between a spherical shell or an ellipsoidal shell by studying the radio images.

The shell model is based on the spherical Hubble flow model as described in Section 2.2 however some additional parameters are introduced. A polar and equatorial direction are defined which, with reference to Figure 2, are along the and axes respectively. The polar velocity, , is greater than the equatorial velocity, , and the two are related by the factor such that  =  . The velocity in these regions is a function of the angle which is defined as

(3)

such that = at = 0 and = at = /2, see Figure 4.

The velocity as a function of is governed by the ellipse equations. In the general case, for an ellipse of semi–major axis , semi–minor axis and eccentricity , the radius as a function of , the angle between the semi–minor and semi–major axes, is given by

(4)

where

(5)

By subtituting Equation 5 into Equation 4 it can be shown that

(6)

and the above formula is used to govern how the velocity varies as a function of in the shell, i.e.

(7)

The elliptical shell models are again constructed based on the best fit parameters of V723 Cas as returned by the light curve fitting in Paper I. The best fitting inner and outer shell velocities are taken to be the velocities of the inner and outer shell boundaries at the pole. The shell mass is taken to be the best fitting shell mass from the spherical model. The value of is arbitrarily chosen to be 0.6 and the inclination of the shell to the plane of the sky is taken to be zero degrees i.e. the shell is viewed ‘side-on’.

Figure 4: Geometry for elliptical shell model.

As with the spherically symmetric model, nine simulated maps are calculated to correspond to the nine epochs of 6 cm MERLIN observations. Equation 7 is used to determine and , the velocities of the inner and outer shell boundaries as a function of , and these velocities are then used to calculate and , the radii of the inner and outer shell boundaries for the specific epoch. The density function

(8)

is then applied to populate the density array in and . Once again the temperature is set at 17000 K within the shell boundaries and is assumed to be 100 K elsewhere.

The nine model intensity distribution maps are presented in Figure 5. As with the spherical case the emission is initially optically thick before expansion causes the optical depth to decrease and the inner shell boundary is revealed. An interesting feature to note is the ‘waist’ of brighter emission in the equatorial region. This is due to the inverse dependence on the quantity in the density equation. This is smaller for small values of than it is for values of close to radians giving rise to a density enhancement near the equator of the shell.

\begin{picture}(10.0,21.0)\put(-3.9,2.79){\special{psfile=ell_no_uv_bw.eps % vscale=80 hscale=80 voffset=1 hoffset=0}} \end{picture}
Figure 5: Model intensity distributions for the elliptical shell model, see Fig. 3.

3 Simulated MERLIN images

Once the model images have been calculated the image files have to be correctly formatted before they can be imported into the National Radio Astronomy Observatory’s Astronomical Image Processing System (AIPS; http://www.aoc.nrao.edu/aips/) which is used to generate the synthetic MERLIN images. A World Coordinate System, frequency and Stokes parameter axes are added. The AIPS task UVCON3 reads the properties of the array from an antenna file and determines the coverage of the interferometer. The visibilities are then calculated from a gridded FFT of a model image. Since the models were defined by fits to the light curve, the flux density is very close to that measured in the actual observations. Gaussian noise is added to the data, the level of which is calculated by UVCON based on integration times and the total length of the track. The data produced by UVCON are deconvolved, cleaned and imaged using IMAGR. In all cases where possible, the imaging process has been consistent with the methods used to produce the 6 cm MERLIN maps shown in Figure 1. The cleaning process was terminated at the first negative clean component and a circular restoring beam of 50 mas was used.

Figure 6 shows the simulated MERLIN images based on the spherically symmetric Hubble flow model. These images are based on a 12 hour track which is of similar length to the original MERLIN observations. The images in Figure 7 take the same model intensity distributions as those used to generate Figure 6 except the simulated coverage is based on a 24 hour track instead of a 12 hour track. Figure 8 shows the model MERLIN observations of the elliptical shell model based on a 12 hour track, and finally Figure 9 shows the same model with a 24 hour track. In each 3 3 grid, left to right, top to bottom, the images correspond to the December 1996, January 1997, March 1998, December 1998, February 2000, April 2000, January 2001, June 2001 and October 2001 MERLIN observations of V723 Cas. Contour levels are (-3, 3, 3, 6, 6, 12, 12…) 0.15 mJy for each image, as quoted in the captions.

4 Discussion

Comparison of Figure 6 to the MERLIN images presented in Figure 1 reveals that even for this simple spherical shell model the similarities between the simulated radio observations and the real MERLIN observations are striking. Initially the source is point-like, not much bigger than the restoring beam. The source expands and as the turn over into optically thin emission begins apparent structure in the shell becomes evident. The source becomes ring-like then divides into the double-peaked structure which is common to all multi-epoch MERLIN observations of classical novae.

\begin{picture}(10.0,21.0)\put(-4.4,-1.5){\special{psfile=sph_nine.ps vscale=1% 20 hscale=120 voffset=1 hoffset=0}} \end{picture}
Figure 6: Simulated radio images for the spherically symmetric Hubble flow model based on a 12 hour track. The contour levels are (-3, 3, 3, 6, 6, 12, 12…) 0.15 mJy.
\begin{picture}(10.0,21.0)\put(-4.2,-1.93){\special{psfile=24nine.ps vscale=13% 0 hscale=130 voffset=1 hoffset=0}} \end{picture}
Figure 7: Simulated radio maps for a 24 hour track of the spherical Hubble flow model. The contour levels are (-3, 3, 3, 6, 6, 12, 12…) 0.15 mJy.
\begin{picture}(10.0,21.0)\put(-3.2,3.2){\special{psfile=ell_nine.eps vscale=8% 0 hscale=80 voffset=1 hoffset=0}} \end{picture}
Figure 8: Simulated radio maps for the elliptical shell model based on a 12 hour track. The contour levels are (-3, 3, 3, 6, 6, 12, 12…) 0.15 mJy.
\begin{picture}(10.0,21.0)\put(-3.2,2.7){\special{psfile=24ell2.eps vscale=80 % hscale=80 voffset=1 hoffset=0}} \end{picture}
Figure 9: Simulated radio maps for the elliptical shell model based on a 24 hour track. The contour levels are (-3, 3, 3, 6, 6, 12, 12…) 0.15 mJy.

The most intriguing feature of these simulated maps is the switching of the alignment of the dominant peaks in the map, giving the impression of rotation. In Paper I we speculated whether this was due to optical depth effects, with higher density regions of the shell remaining optically thick for longer and appearing as peaks of radio emission as the photosphere recedes. Here this explanation can be ruled out as the mass distribution supplied by the model is spherical with a smooth radial density profile.

Comparing Figure 7 to Figure 6, shows that for a 24 hour observation the radio emission in the synthetic maps is more circularly symmetric and consquently more faithful to the model images. The effect whereby the alignment of the dominant peaks in emission appears to rotate between epochs is also almost completely eradicated. The increase in coverage provided by the 24 hour observation must be the reason for this, providing both an improved signal to noise ratio and a drastically altered sidelobe structure in the beam. The beam shape and coverage are discussed in Section 4.1. Table 1 lists the root mean square values of the background noise for both 12 and 24 hour tracks of the simulated spherical Hubble flow model.

Epoch 12 hour track 24 hour track
Dec 96 0.169 0.124
Jan 97 0.129 0.119
Mar 98 0.177 0.137
Dec 98 0.185 0.141
Feb 00 0.141 0.134
Apr 00 0.137 0.133
Jan 01 0.136 0.124
Jun 01 0.131 0.117
Oct 01 0.128 0.112
Table 1: Comparison of the background rms values in mJy/beam for both the 12 and 24 hour simulations of the spherical Hubble flow model.

The simulated radio maps for the ellipsoidal shell model reveal a north–south bias with a double peaked source being present for the first five epochs. This gives way to a ‘partial shell’ structure which in turn is replaced by the east–west aligned peaks in the final map. Although a stronger north–south alignment of the emission would be expected from this ellipsoidal shell model the evolution of the radio emission over time displays many similiarities to the spherical case. Both initially develop a north–south bias which gives way to an east–west alignment and although this process occurs later for the ellipsoidal shell it is unlikely that a 12 hour track can be used to distinguish between an ellipsoidal or a spherical shell for objects of this nature.

In order to determine whether a 24 hour track would produce a distinction between ellipsoidal and spherical shells the simulations presented in Figure 9 can be examined. For the optically thick stage the MERLIN images accurately represent the simulated brightness distributions but for subsequent epochs the images detect only the brighter east-west aligned emission around the inner shell boundary. The faint, extended structure along the major axis of the shell is below detectability. With a greater signal to noise ratio, or alternatively an object brighter than V723 Cas, it is likely that observations based on a 24 hour track could be used to examine the eccentricity of an ellipsoidal shell.

4.1 Comparing the beams and the coverage

Figure 10 shows the improved coverage of the 24 hour track compared to the 12 hour track. Plots of the beam shape for both 12 and 24 hour observations are presented in Figure 11. Immediately apparent is the effect that the increased coverage has on the sidelobes of the beam. The sidelobe structure in the 24 hour observation completely surrounds the central maximum and only deviates from circularity due to the declination of the source. The beam of the 12 hour simulation has -shaped sidelobe structure. As the source expands through the beam different parts of the shell will be buried in the sidelobes. The non-circular beam shape associated with the 12 hour track could be a possible cause for the apparent rotation of the nova shell between different epochs. Since this effect is generally not an issue with observations involving strong sources on larger scales (e.g. radio galaxies) it is likely that these effects will only be present when observing objects with low surface brightness objects and small angular sizes, and would probably pass unnoticed when observing systems with less favourable dynamic timescales. Additionally a 24 hour track provides higher fidelity images due to more thorough sampling of the plane and an improved signal to noise ratio.

Figure 10: Plots of the simulated coverage for a 12 hour (upper panel) and 24 hour (lower panel) track.
Figure 11: Plots of the beam structure for the simulated 12 hour (upper panel) and 24 hour (lower panel) observations. The beam structure is shown on the same scale as the simulated radio images.

4.2 Rings and discs

The Fourier transform process can give rise to unexpected artefacts in the final image. In this section we briefly investigate the possibility that the transition from a disc shaped structure to something that is ring-like could be responsible for unusual effects in the final radio images. Examination of Figure 3 shows how the model emitting region develops with time. Initially the source is optically thick and resembles a disc on the sky, with the flux density at this stage governed only by the angular size and the brightness temperature. The highest contour level also drifts around the field as the shell expands. Later a transition to optically thin emission occurs and the ring-like inner shell boundary is revealed. In order to assess the outcome of this transition on the final radio images, simulated MERLIN observations of an expanding ring are presented for comparison with those of an expanding disc. These are presented in Figures 12 and 13.

The model emitting region in each case has angular size scales and flux densities comparable with that of the shell of V723 Cas. As the intention here is to solely investigate the effect of the deconvolution process the final simulated data do not have Gaussian noise added. Note the differing contour levels for the ring and disc maps. The disc simulation is plotted with levels of (-3, 3, 3, 6, 6, 12, 12…) 0.15 mJy as with the real MERLIN maps and the simulations presented in this paper. Since the simulated ring structure is much fainter the contour levels are reduced to (-3, 3, 3, 6, 6, 12, 12…) 0.03 mJy. The disc simulation is brighter simply because there is more emitting material.

Figure 12: Synthetic 12 hour MERLIN observations of an expanding ring.
Figure 13: Synthetic 12 hour MERLIN observations of an expanding disc.

Examination of Figures 12 and 13 reveals that even these simple zero noise models exhibit features such as apparent rotation and peaks dividing as the emitting region expands. These effects are seen in both the ring and the disc model meaning that it is unlikely that they appear in the real observations due to the nova undergoing the transition from disc-like to ring-like. This is further evidence that these effects are due to the limited coverage and are not related to the changing optical depth or other underlying properties of the source.

5 Conclusions

These results have shown that extreme care must be taken when using radio images alone to interpret the morphology of classical nova shells such as that of V723 Cas. The (comparatively) low radio surface brightness of a nova shell coupled with its low angular size gives makes it prone to instrumental effects which may be mistaken for unusual shell morphology and motion (e.g. clumping, apparent rotation). However these effects can be mitigated by using observations with longer tracks which both improves the coverage and increases the signal to noise ratio. When using radio imaging to track structure in novae and similar objects, coupling of simulations such as those presented here with observations would provide a more thorough insight into the underlying source structure.

However, optical imaging of novae reveal that the emission is far from homogeneous and exhibits equatorial and polar enhancements (e.g. FH Ser, Gill & O’Brien, 2000), clumping of material and even filamentary structures (e.g. GK Per, Slavin et al, 1995). Thus there is need for spherical models to be refined and it will be interesting to see how novae are observed by the next generation of interferometers such as -MERLIN. With the vastly improved plane sampling of -MERLIN exploiting multifrequency synthesis, Figure 14, one would not expect the instrumental effects documented in this paper to be present. Preliminary simulations shown in Figure 15 show three epochs of the elliptical shell model described in Section 2.3. Immediately apparent is the north-south aligned, extended, low brightness emission which was below detectability levels in the simulations presented in Section 3. The root mean square background noise levels in the -MERLIN simulations are Jy. The plane sampling is consistent with that of -MERLIN observing using a 5 GHz contiguous band, i.e. 1000 frequency channels between 2 GHz and 5 GHz. The drawback here is that these simulations treat the source as being spectrally flat, which is obviously a poor assumption over such a wide frequency range. Nonetheless they show that the -MERLIN view of sources of this nature will be much more faithful to the true source distribution due to its vastly improved coverage and sensitivity.

Figure 14: Simulated coverage of a 12 hour track using the -MERLIN 5 GHz contiguous band.
Figure 15: Preliminary -MERLIN simulations of the December 1996, December 1998 and October 2001 epochs of the elliptical shell model.

Acknowledgements

IH wishes to thank the Particle Physics and Astronomy Research Council (PPARC). MERLIN is operated as a UK National Facility by the University of Manchester, Jodrell Bank Observatory, on behalf of PPARC. IH also thanks Simon Garrington for his valuable input. This research has made use of NASA’s Astrophysics Data System. The authors wish to thank the reviewer, Amy Mioduszewski, for her constructive criticisms.

Footnotes

  1. pagerange: Simulations and interpretation of the 6 cm MERLIN images of the classical nova V723 CasSimulations and interpretation of the 6 cm MERLIN images of the classical nova V723 Cas
  2. pubyear: 200x
  3. Recently a bug was discovered in the AIPS task UVCON whereby in certain cases visibilities in the simulated data set would be recorded with telescopes at negative elevations, and then conversely visibilities would be missing from high elevations where they should be present (L. Kogan, private communication). When this problem came to light the simulations in this paper were naturally re-examined to check for this problem. This footnote is merely to confirm that the results presented are not affected. The declination of V723 Cas coupled with the latitudes of the stations in the MERLIN array result in positive elevations throughout, even for a 24 hour track.

References

  1. Dougherty, S. M., Pittard, J. M., Kasian, L., Coker, R. F., Williams, P. M., & Lloyd, H. M. 2003, A&A, 409, 217
  2. Eyres S.P.S., Davis R.J., Bode M.F., 1996, MNRAS, 279, 249
  3. Eyres S.P.S., Bode M.F., O’Brien T.J., Watson S.K., Davis R.J., 2000, MNRAS, 318, 1086
  4. Eyres, S. P. S., Heywood, I., O’Brien, T. J., Ivison, R. J., Muxlow, T. W. B., & Elkin, V. G. 2005, MNRAS, 358, 1019
  5. Gill, C. D., & O’Brien, T. J. 2000, MNRAS, 314, 175
  6. Heywood, I., O’Brien, T. J., Eyres, S. P. S., Bode, M. F., & Davis, R. J. 2002, AIP Conf. Proc. 637: Classical Nova Explosions, 637, 242
  7. Heywood, I., O’Brien, T. J., Eyres, S. P. S., Bode, M. F., & Davis, R. J. 2005, MNRAS, 362, 469
  8. Hjellming R.M., Wade C.M., Vandenberg N.R., Newell R.T., 1979, AJ, 84, 1619
  9. Seaquist E.R., Palimaka J., 1977, ApJ, 217, 781
  10. Slavin, A. J., O’Brien, T. J., & Dunlop, J. S. 1995, MNRAS, 276, 353
  11. Starrfield S., 1989, in Bode M.F., Evans A., eds, Classical Novae. Wiley, Chichester, p. 39
  12. Taylor A.R., Pottasch S.R., Seaquist E.R., Hollis J.M., 1987, A&A, 183, 38
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minumum 40 characters
Add comment
Cancel
Loading ...
106319
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description