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We adopted the usual Henyey–Greenstein (1941) phase function. Figure 11. In 1988, a luminous cool object appeared in the nuclear bulge of M31. The angular diameter of the linear-polarization ring in a SN light echo (corresponding to a linear diameter of 2ct) is given by θ = 0'126(t/1 yr)(1 Mpc/D). Anticipating the results below, we show the locations of the light-echo paraboloids for an assumed distance of 6.1 kpc. The Hubble telescope has imaged V838 Mon and its light echo several times since the star's outburst. The outburst mechanism for this new class of objects remains uncertain. Figure 4 shows the result of masking out regions with S/N < 10 and regions near bright stars, as described above, for each of the four epochs. 0000003625 00000 n
The high luminosities and rapid expansion timescales appear to disallow a "born-again" event in a low-mass pre-white dwarf. (2005). We compared the full azimuthally averaged polarimetric data to model polarization curves determined numerically as described in Section 4, for a range of assumed distances D and fitting pmax as a free parameter. Measurements of the star’s light output showed that the explosion happened in three stages, flaring and then dimming three times from January to March 2002. The dotted curve is the analytic solution for an instantaneous outburst with D90 = 6.1 kpc. j�t��+�w��+�F*�*U[{���B/��n.�Tby�n��铴�ga*�9�ἱ�x��P�1�q#~�Op� �F2V/�v2��͆f�կ7Z������B�k��gF|�� �c&l�+��'�7Pg�?�@ �����^������N��I�u
�t���ĉ�Ito�����,FY(-L`]ǭ� ����b��H#���S�a�J�O���/&t���&����!BK"z<>?\���1!����Y�dhyczO�����h�HƯ�O!�+��3�~Ώ���������"@ �` ����?ڎR�6��F��>��\�,�ؕ7���خ1�5�. Table 3. The image stretch is linear, and the fading of the light echo has been compensated by scaling the image intensities. To test the robustness of this approach, and reduce sensitivity to the shape of the broad, low-polarization wings, we also derived rms residuals restricting the models and data just to regions where the polarization degree was greater than 0.4, i.e., fitting the models just to the peak of the curve. (2004, their Table 19). S = 15 Mon falls among the stars of the young cluster NGC 2264, is surrounded by a bright nebula called Sharpless 273, which it helps excite, and lies to the north of one of the fantastic sights of the sky, the “Cone Nebula,” a long dark interstellar dust cloud that is being evaporated at its tip by another nearby hot star. The local standard deviation of the sky was consistent with our noise model; however there were small but significant differences between the 12 measurements, corresponding to fluctuations in the background of ~3%–5%. Beyond the stellar image cores, in the region where the halo has less than a 10% influence on polarization, we subtracted the estimated stellar halo from the Stokes I image and corrected the polarization-degree image accordingly for this small effect. A light echo provides the possibility of direct geometric distance determination, because it should contain a ring of highly linearly polarized light at a linear radius of ct, where t is the time since the outburst. Setting the radius of this ring to a linear size of ct yielded initial distance estimates of 5.4–6.2 kpc. 2002 and references therein). The actual data are shown as noisy curves.
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