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Finally. Sevtert Is are ttose Objects where none of the three materials intercepts the line of sight.
Finally, Seyfert 1s are those objects where none of the three materials intercepts the line of sight.
However. cdepeuding ou the ecometiy ixl covering factor of the imer absorber. they lay occasionally show even rapid parlal or total occultation events.
However, depending on the geometry and covering factor of the inner absorber, they may occasionally show even rapid partial or total occultation events.
Tudeed. this ds he case of NGC 1051 (?).. NGC 3227 (2) NAyk 335 (7) aud II0557-385 (?)..
Indeed, this is the case of NGC 4051 \citep{gua98}, NGC 3227 \citep{lamer03} Mrk 335 \citep{gkg07} and H0557-385 \citep{long08}.
While iu some cases all alternative sohtion iu ternis of cswitchine-off” of the source is equally viable. iu fje last two cases the partial covering from au intervene absorber is preferred.
While in some cases an alternative solution in terms of `switching-off' of the source is equally viable, in the last two cases the partial covering from an intervening absorber is preferred.
Even if the timescales are uot particularly coustraiine. the presence of wart absorption signatures muchaiced: between the two states of IT(0557-385 strongly suggestsOO hat the neutral absorbiis clouds are locaed close to the BIL iu agreement with the precoc.ctions of the model proposed iu his oper.
Even if the timescales are not particularly constraining, the presence of warm absorption signatures unchanged between the two states of H0557-385 strongly suggests that the neutral absorbing clouds are located close to the BH, in agreement with the predictions of the model proposed in this paper.
We note here hat sinultaneous optica ancl N-ray campaiens oftlose sources would be revealing for the exact location of the absorber with resect to the BER. looking for the presence of POAC optical lines during the N-rav absorption states,
We note here that simultaneous optical and X-ray campaigns of these sources would be revealing for the exact location of the absorber with respect to the BLR, looking for the presence of broad optical lines during the X-ray absorption states.
While the study. of he nature of this iuner absorber is well bevoud t16 scope of this paper. we note here that this scenario is well in agreement with theoretical models which sueeestOO a stroug link. both geometrical axd plixsical. between the
While the study of the nature of this inner absorber is well beyond the scope of this paper, we note here that this scenario is well in agreement with theoretical models which suggest a strong link, both geometrical and physical, between the
We discuss the application of LAE to pulsars. both as a high-enerey emission process and as a Maser emission process at radio frequencies.
We discuss the application of LAE to pulsars, both as a high-energy emission process and as a maser emission process at radio frequencies.
Our conclusions are:
Our conclusions are:
AL.. we estimate a SFR [or massive stars of SFRoajm (AL=SAL. )=470hz AL. veth
$_{\sun}$, we estimate a SFR for massive stars of $_{60\,\mu \rm{m}}$ $\rm{M} \geq 5\,\rm{M}_{\sun}$ $=470~h_{65}^{-2}$ $_{\sun}$ $^{-1}$.
Alternatively. from the observed radio power (Pyicu;=15xLo?!hz !) we deduce pou, (Al>5M.)2 377hz M. ft. consistent with the value estimated from the GO jan. luminosity.
Alternatively, from the observed radio power $_{1.4\,\rm{GHz}} = 1.5 \times\ 10^{24}~h_{65}^{-2}$ $^{-1}$ ) we deduce $_{1.4\,\rm{GHz}}$ $\rm{M} \geq 5\,\rm{M}_{\sun}$ $=377~h_{65}^{-2}$ $_{\sun}$ $^{-1}$, consistent with the value estimated from the 60 $\mu$ m luminosity.
On the other hand. the extinetion-corrected Ho luminosity (Lin,=0.9—2.6x107.5,2 W) implies SFR(M ο j=620ΠΟ... the large range being due to the unresolved contribution of [NII] to the observed Ia [NI] blend.
On the other hand, the extinction-corrected $\alpha$ luminosity $_{\rm{H}\alpha} = 0.9-2.6\times 10^{37}~h_{65}^{-2}$ W) implies $_{\rm{H}\alpha}$ $\rm{M} \geq 5\,\rm{M}_{\sun}$ $=620-1730~h_{65}^{-2}$ $_{\sun}$ $^{-1}$, the large range being due to the unresolved contribution of [NII] to the observed $\alpha$ +[NII] blend.
This excess over the SFR estimated [rom FIR and radio luminosities may be due to ihe AGN contribution.
This excess over the SFR estimated from FIR and radio luminosities may be due to the AGN contribution.
Three other dusty ERGs have been spectroscopically confirmed and are relatively well studied: IIRTO. displaying strong starburst activity al z=1.44 (Devefaf.1999): 2016. à 2=1.50 galaxy which hosts a dusty quasar (Pierreefaf,2001) and EROJ164023. which at 2=1.05 shows star-forming activity with a possible weak AGN (Smithe£al.2001).
Three other dusty ERGs have been spectroscopically confirmed and are relatively well studied: HR10, displaying strong starburst activity at $z=1.44$ \citep{Dey99}; ISOJ1324-2016, a $z=1.50$ galaxy which hosts a dusty quasar \citep{Pie01} and EROJ164023, which at $z=1.05$ shows star-forming activity with a possible weak AGN \citep{Smi01}.
. A brief comparison of some of the observed quantities in PDEJOL1423 and these three other dusty ERGs is listed in Table 2.
A brief comparison of some of the observed quantities in PDFJ011423 and these three other dusty ERGs is listed in Table 2.
Although the non detection of star formation in can be due to the lack of FUR/sub-mmnm observations. it seems clear that dillerent degrees ol AGN and starburst activitv do exist in the dusty ERG population.
Although the non detection of star formation in ISOJ1324-2016 can be due to the lack of FIR/sub-mm observations, it seems clear that different degrees of AGN and starburst activity do exist in the dusty ERG population.
Given the lower recshilt of PDEJOII423. this source offers the best opportunity to study the interplay between the two phenomena in the dusty environments of these galaxies.
Given the lower redshift of PDFJ011423, this source offers the best opportunity to study the interplay between the two phenomena in the dusty environments of these galaxies.
The ratio of the radio power to the dust-corrected optical Iuminosityx of PDEJOL12423. πιLp~1. confinns that PDEJOI11422 is radio «quiet.
The ratio of the radio power to the dust-corrected optical luminosity of PDFJ011423, $P_{1.4}/L_R \sim 1$, confirms that PDFJ011423 is radio quiet.
It seems likely (hat this source is linked to the racdio-quiel counterparts of the red quasar population discovered by (1995). and also to the ERGs recently discovered among the population responsible for the hard X-ray background (ILasingere£aL2001).
It seems likely that this source is linked to the radio-quiet counterparts of the red quasar population discovered by \citet{Web95} and also to the ERGs recently discovered among the population responsible for the hard X-ray background \citep{Has01}.
. Future work will show if the intense star formation activity present in PDEJO11423 is also a common feature to the above mentioned obseured AGN populations.
Future work will show if the intense star formation activity present in PDFJ011423 is also a common feature to the above mentioned obscured AGN populations.
All these different. studies suggest the existence of an important population of dusty. ERGs. powered by heavily obscured starbursts and/or AGNs. which is now starting to be observed.
All these different studies suggest the existence of an important population of dusty ERGs, powered by heavily obscured starbursts and/or AGNs, which is now starting to be observed.
Given their extreme nature. the study of the custy ERGs will hold funcamental clues to the understanding of galaxy evolution. by revealing valuable information on the hidden star formation and AGN activity in the universe.
Given their extreme nature, the study of the dusty ERGs will hold fundamental clues to the understanding of galaxy evolution, by revealing valuable information on the hidden star formation and AGN activity in the universe.
We are grateful to A. Verma for adapting and running her SED fitting algorithm for this source and for useful discussions.
We are grateful to A. Verma for adapting and running her SED fitting algorithm for this source and for useful discussions.
We also thank A. Efstathiou and M. Rowan-Robinson for (heir advice.
We also thank A. Efstathiou and M. Rowan-Robinson for their advice.
The aware of the European Southern Observatory Directors discretionary time is gratefully acknowledged.
The award of the European Southern Observatory Director's discretionary time is gratefully acknowledged.
JA eratefullv acknowledges a scholarship from the Science and Technology Foundation (FCT. Portugal) and the assistance [rom the Universitv of London
JA gratefully acknowledges a scholarship from the Science and Technology Foundation (FCT, Portugal) and the assistance from the University of London
the energy at which resonant mode conversion becomes effective.
the energy at which resonant mode conversion becomes effective.
For B=7x1015 G, the vacuum resonance density is nearly equal to the O mode decoupling density, depending on the NS rotational phase.
For $B = 7\times 10^{13}$ G, the vacuum resonance density is nearly equal to the O mode decoupling density, depending on the NS rotational phase.
For most values of w, p=py is within the X and O mode photospheres, and no rotation of the plane of polarization occurs.
For most values of $\psi$, $\rho = \rho_V$ is within the X and O mode photospheres, and no rotation of the plane of polarization occurs.
Thus, Qaye retains the same sign at low and high energies (c.f.,figure20of?,forasimilargeometry )..
Thus, $Q_{\rm ave}$ retains the same sign at low and high energies \citep[c.f., figure~20 of][for a similar result in a different geometry]{vanAdelsbergLai06a}.
Magnetar atmospheres are typically assumed to consist of mostly hydrogen.
Magnetar atmospheres are typically assumed to consist of mostly hydrogen.
However, if hydrogen is depleted by thermonuclear burning in the photosphere, they may consist of helium (?)..
However, if hydrogen is depleted by thermonuclear burning in the photosphere, they may consist of helium \citep[][]{Changetal04a}. .
For fully ionized helium composition at B=5x1014 G, and Tyg=5x106 K, we find that the observed Stokes parameters differ from those in the hydrogen case by —1096 for 0.1«E10 keV. We therefore do not show results for this case.
For fully ionized helium composition at $B=5\times 10^{14}$ G, and $T_{\rm eff} = 5\times 10^6$ K, we find that the observed Stokes parameters differ from those in the hydrogen case by $\la 10\%$ for $0.1 < E < 10$ keV. We therefore do not show results for this case.
The reason for the similarity is that the O mode decoupling depth in ionized helium is ~60% of that in hydrogen, while the vacuum resonance density (identified with the X mode decoupling depth at large magnetic field strengths) increases bya factor of two.
The reason for the similarity is that the O mode decoupling depth in ionized helium is $\sim 60\%$ of that in hydrogen, while the vacuum resonance density (identified with the X mode decoupling depth at large magnetic field strengths) increases bya factor of two.
The temperature profile
The temperature profile
The right panel of Fig.
The right panel of Fig.
6 shows the relationship between log(c) and log(Z,)y for pseudo- and classical bulges.
6 shows the relationship between $\log \left<\sigma_\star\right>$ and $\log \left<Z_\star\right>_M$ for pseudo- and classical bulges.
This relation also flattens out at high (c) end, similar to that between Mijp and log(Z.)y.
This relation also flattens out at high $\left<\sigma_\star\right>$ end, similar to that between $M_{i,\,{\rm B}}$ and $\log \left<Z_\star\right>_M$.
It is not unreasonable because both M;pg and (σα) can trace the stellar mass for a more fundamental relation, the stellar mass-metallicity relation.
It is not unreasonable because both $M_{i,\,{\rm B}}$ and $\left<\sigma_\star\right>$ can trace the stellar mass for a more fundamental relation, the stellar mass-metallicity relation.
The distribution of pseudo- and classical bulges in the σι—Z, plot further confirms that pseudo- and classical bulges have different mean stellar metallicities may be simply due to they having different stellar masses.
The distribution of pseudo- and classical bulges in the $\sigma_\star-Z_\star$ plot further confirms that pseudo- and classical bulges have different mean stellar metallicities may be simply due to they having different stellar masses.
The fraction distributions of the velocity dispersions for pseudo-bulges and classical bulges are plotted in the left panel of Fig.
The fraction distributions of the velocity dispersions for pseudo-bulges and classical bulges are plotted in the left panel of Fig.
7.
7.
From the figure we can see that about a half of the sampled pseudo-bulges have their σεXCinst, which will result in a serious uncertainty.
From the figure we can see that about a half of the sampled pseudo-bulges have their $\sigma_\star \lesssim \sigma_{\rm{inst}}$, which will result in a serious uncertainty.
However, these measurements are still used as a very rough estimation, and it will not affect our main conclusion that classical bulges have larger velocity dispersions than pseudo-bulges (see Fig.
However, these measurements are still used as a very rough estimation, and it will not affect our main conclusion that classical bulges have larger velocity dispersions than pseudo-bulges (see Fig.
7) in our sample.
7) in our sample.
As shown in Table 1, the mean values of the velocity dispersions for pseudo ((σκ)ρ) and classical (a7, ),) bulges are 72.4+16.2kms! and 116.6::34.8kms!, respectively.
As shown in Table 1, the mean values of the velocity dispersions for pseudo $\left<\sigma_\star\right>_{\rm{p}}$ ) and classical $\left<\sigma_\star\right>_{\rm{c}}$ ) bulges are $72.4\pm16.2\,{\rm{km\,s^{-1}}}$ and $116.6\pm34.8\,{\rm{km\,s^{-1}}}$, respectively.
One characteristic of pseudo-bulges is their positions with respect to the Faber-Jackson relation (FJ;Faber&Jackson 1976),, which is a correlation between the central velocity dispersion of elliptical galaxies/bulges and their luminosity.
One characteristic of pseudo-bulges is their positions with respect to the Faber-Jackson relation \citep[FJ;][]{fab76}, , which is a correlation between the central velocity dispersion of elliptical galaxies/bulges and their luminosity.
Kormendy&Kennicutt(2004) show that pseudo-bulges fall well below this relation.
\cite{kor04} show that pseudo-bulges fall well below this relation.
In the right panel of Fig.
In the right panel of Fig.
7, we show the relation between the velocity dispersion and absolute magnitude for all bulges, with the solid line showing the SDSS i-band result from LaBar-beraetal.(2010) for early type galaxies.
7, we show the relation between the velocity dispersion and absolute magnitude for all bulges, with the solid line showing the SDSS $i$ -band result from \cite{lab10} for early type galaxies.
We can see from the figure that, most pseudo-bulges are indeed below the FJ relation, which suggests that they have a lower velocity dispersion comparing to their classical counterparts.
We can see from the figure that, most pseudo-bulges are indeed below the FJ relation, which suggests that they have a lower velocity dispersion comparing to their classical counterparts.
Therefore, our result confirms the general finding that classical bulges are more dispersion-supported than pseudo-bulges.
Therefore, our result confirms the general finding that classical bulges are more dispersion-supported than pseudo-bulges.
In this paper we present the stellar population synthesis results for a sample of 75 isolated classical bulges and pseudo-bulges, using the SDSS spectra and the STARLIGHT code.
In this paper we present the stellar population synthesis results for a sample of 75 isolated classical bulges and pseudo-bulges, using the SDSS spectra and the STARLIGHT code.
For this sample we find that the stellar population of pseudo-bulges is, in general, younger and less abundant in metal than that of classical bulges, while these differences are not significant, and both types of bulges are predominantlyli composed of old stellar populations, with mean mass- stellar age around 10 Gyr.
For this sample we find that the stellar population of pseudo-bulges is, in general, younger and less abundant in metal than that of classical bulges, while these differences are not significant, and both types of bulges are predominantly composed of old stellar populations, with mean mass-weighted stellar age around 10 Gyr.
The apparent lower
The apparent lower
typically much cooler than this. averaging ouly 16000 kelvin (Sion1999).
typically much cooler than this, averaging only $\sim 16000$ kelvin \citep{sion99}.
. On both these groiuds it seems uulikely that a normal white cwarl is poweriug the heating eleet.
On both these grounds it seems unlikely that a normal white dwarf is powering the heating effect.
The implied uass Is large because the heating 11odel requires a ow inclination.
The implied mass is large because the heating model requires a low inclination.
One natural stigegestion lor iuc‘easine 7. hei'e lowering My. is to :vdd a sourcee of steady light to tlie system. as would be expectec Lf'om the primary.
One natural suggestion for increasing $i$ , hence lowering $M_1$, is to add a source of steady light to the system, as would be expected from the primary.
However. as noed earlier. the observed colors from the near ultraviolet to the nid-iufrared are all nicely matched N pure Ci-star amospheres.
However, as noted earlier, the observed colors from the near ultraviolet to the mid-infrared are all nicely matched by pure G-star atmospheres.
We tried addiug light artificially. all of course this increased the ineination. but unless the added light was also tuned to be alios exactly tlie €olor of the secoucary. the added light «estroved the color match.
We tried adding light artificially, and of course this increased the inclination, but unless the added light was also tuned to be almost exactly the color of the secondary, the added light destroyed the color match.
In particular. adding aiv siguilicaut amount of light similar in color to a hot white dwarf completely destroved the agreetvent between the observed ancl modeled colors.
In particular, adding any significant amount of light similar in color to a hot white dwarf completely destroyed the agreement between the observed and modeled colors.
What are we to make of this star?
What are we to make of this star?
Except for the unusual discovery channel. the evidence available to Bondetal.(2002) showed a typical AM Her-ype cataclysmic binary. vet since then it has shown a very different face. most likely because mass transfer has ceased. at least for the time being.
Except for the unusual discovery channel, the evidence available to \citet{bond} showed a typical AM Her-type cataclysmic binary, yet since then it has shown a very different face, most likely because mass transfer has ceased, at least for the time being.
There is nothing in the miuimun-light spectrum to suggest it is a cataclysmic binary: in particular there are io eiission lines.
There is nothing in the minimum-light spectrum to suggest it is a cataclysmic binary; in particular there are no emission lines.
Even at deep mitnui. ANI Her stars such as EF Eri still low eluission (see. e.g.. Wheatey&Ratsay 1998)).
Even at deep minimum, AM Her stars such as EF Eri still show emission (see, e.g., \citealt{wheatley98}) ).
The early spectral type oftie secoudary is also unusua.
The early spectral type of the secondary is also unusual.
Beuerinanuetal.(1998) compiled the »ectral types of CV secondaries as a function of pP4. aud found that for orbital periods 2,4,ori<3 hr. early all were consistent with 1ialu-sequeuce expectations. whüle for Py,>3 hir. secondaries were either near the main sequence orcooler than expected.
\citet{beuermann2ndry} compiled the spectral types of CV secondaries as a function of $_{\rm orb}$, and found that for orbital periods $P_{\rm orb} < 3$ hr, nearly all were consistent with main-sequence expectations, while for $P_{\rm orb} > 3$ hr, secondaries were either near the main sequence or than expected.
At the L75 hr period of FIRST 10234-0038. je. spectral type of a secouclaΝ obeyiug the main-sequence 1jass/Taclius/spectral-type relation would be near M2. cooler than observed. so FIRST 10232-0038 lies on the wrong side of the eid liue.
At the 4.75 hr period of FIRST 1023+0038, the spectral type of a secondary obeying the main-sequence mass/radius/spectral-type relation would be near M2, cooler than observed, so FIRST 1023+0038 lies on the `wrong' side of the trend line.
Recently. Thorsteuseretal.(2002a) and Thorsteuseretal.(2002b) drew attention to wo shorer-period systems that also show anomalously warn secoudaries. namely EI UMa (P=61 uin) aud QZ Ser (P=2.0 hr).
Recently \citet{thorstensenei} and \citet{thorstensenqz} drew attention to two shorter-period systems that also show anomalously warm secondaries, namely EI UMa $P = 64$ min) and QZ Ser $P = 2.0$ hr).
The explanation acdvaucec iu tlOse papers was that these objects arose [rou svsteis in which mass trausfer began after the secordary had uudergoue some nuclear evolutior.
The explanation advanced in those papers was that these objects arose from systems in which mass transfer began after the secondary had undergone some nuclear evolution.
In QZ Ser. this is corroborated by au apparent enliux'ement of the Na abundauce. since Nals bred out of Ne at temperatures consistent with H burning i the CNO evele.
In QZ Ser, this is corroborated by an apparent enhancement of the Na abundance, since Na is bred out of Ne at temperatures consistent with H burning in the CNO cycle.
The early spectral type ale stroug NaD line in FIRST 10234-0038 suggest that 1ie secondary has uudergone some liciearevolution in this system as well.
The early spectral type and strong NaD line in FIRST 1023+0038 suggest that the secondary has undergone some nuclear evolution in this system as well.
The Boudetal.(2002) spectrum does slow H emission. so H-burui[n]ο evideutlv did not complete iu the material that is presently exposed on the secondarys surface.
The \citet{bond} spectrum does show H emission, so H-burning evidently did not complete in the material that is presently exposed on the secondary's surface.
The lack of emissiou lines and the excellent fit to a pure heating-ellect light curve at. low inclination preseuts the most severechallenges to uuderstaudiug.
The lack of emission lines and the excellent fit to a pure heating-effect light curve at low inclination presents the most severechallenges to understanding.
Here are [our scenarios which uiieght explain the observations.
Here are four scenarios which might explain the observations.
2007).
.
. This is at the S/N = 5 detection limit of LISA alter 1 vear of observations.
This is at the S/N = 5 detection limit of LISA after 1 year of observations.
We report the discovery of a new 40 min orbital period cetached binary WD system. J1630.
We report the discovery of a new 40 min orbital period detached binary WD system, J1630.
Alone with the previously discovered. 12 min and 39 min orbital period systems. J0651 and JOLOG. 1630 is only the third. known detached binary WD system with a period less than an hour.
Along with the previously discovered 12 min and 39 min orbital period systems, J0651 and J0106, J1630 is only the third known detached binary WD system with a period less than an hour.
All three systems are excellent gravitational wave sources to be detected by LISA.
All three systems are excellent gravitational wave sources to be detected by LISA.
J1630 is almost a twin of the 39 min orbital period system JOLOG.
J1630 is almost a twin of the 39 min orbital period system J0106.
Llowever. due to its smaller size and larger mass. significant ellipsoidal variations are neither expected nor detected in its light curve.
However, due to its smaller size and larger mass, significant ellipsoidal variations are neither expected nor detected in its light curve.
Fherefore. the inclination angle. of the system cannot be constrained. accurately with the current data.
Therefore, the inclination angle of the system cannot be constrained accurately with the current data.
Follow-up. high-speed photometric observations at a larger telescope will be useful to constrain the doppler boosting signal more accurately ancl to search for grazing eclipses.
Follow-up high-speed photometric observations at a larger telescope will be useful to constrain the doppler boosting signal more accurately and to search for grazing eclipses.
The two WDs in this svstem will merge in less than 31 Myr and likely form a single subclwarl star or a rapidly rotating massive WD.
The two WDs in this system will merge in less than 31 Myr and likely form a single subdwarf star or a rapidly rotating massive WD.
We thank D. Koester for. kindly providing WD. moclel spectra.
We thank D. Koester for kindly providing WD model spectra.
DEW and JIL gratefully acknowledge the support of the NSF under grant AST-00091€C) and the Norman llackerman Advanced Research Program uncer grants 003658-0255-2007 and 003658-0252-2009.
DEW and JJH gratefully acknowledge the support of the NSF under grant AST-0909107 and the Norman Hackerman Advanced Research Program under grants 003658-0255-2007 and 003658-0252-2009.
processed to remove the sky background.
processed to remove the sky background.
An object-finding algorithm was used to locate and classify the stars and galaxies in the fields.
An object-finding algorithm was used to locate and classify the stars and galaxies in the fields.
The stars were then matched and calibrated against the USNO A1.0 catalog (Monetetal.1996) to derive a magnitude zeropoint for each image.
The stars were then matched and calibrated against the USNO A1.0 catalog \citep{usnoa1} to derive a magnitude zeropoint for each image.
There were typically a few hundred USNO ΑΙ.0 stars in each 0.25 iimage.
There were typically a few hundred USNO A1.0 stars in each 0.25 image.
The supernova was discovered by subtracting PSF-matched historical NEAT images from new images, then automatically detecting residual sources for subsequent human inspection (see Wood-Vaseyetal. (2004))).
The supernova was discovered by subtracting PSF-matched historical NEAT images from new images, then automatically detecting residual sources for subsequent human inspection (see \citet{wood-vasey04}) ).
For analysis, we assembled all NEAT images, including later images kindly taken at our request by the NEAT team.
For analysis, we assembled all NEAT images, including later images kindly taken at our request by the NEAT team.
Light curves were generated using aperture photometry scaled to the effective seeing of each image.
Light curves were generated using aperture photometry scaled to the effective seeing of each image.
A set of the 4 best-seeing (< 3")) reference images was selected from among all NEAT Palomar pre-explosion images from 2001 of SN 2002ic.
A set of the 4 best-seeing $<3$ ) reference images was selected from among all NEAT Palomar pre-explosion images from 2001 of SN 2002ic.
Multiple reference images were chosen to better constrain any underlying galaxy flux.
Multiple reference images were chosen to better constrain any underlying galaxy flux.
The differential flux in an aperture around SN 2002ic was measured between each reference image and every other image of SN 2002ic.
The differential flux in an aperture around SN 2002ic was measured between each reference image and every other image of SN 2002ic.
Aperture correction was performed to account for the different seeing and pixel scales of the images.
Aperture correction was performed to account for the different seeing and pixel scales of the images.
The overall flux ratio between each reference image and light-curve image was tracked and normalized with respect to a primary reference image.
The overall flux ratio between each reference image and light-curve image was tracked and normalized with respect to a primary reference image.