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A number of interesting astronomy targets have been observed. during the OSCA commissioning runs. | A number of interesting astronomy targets have been observed during the OSCA commissioning runs. |
The most »ositive results were the very faint detection of the cool white dwarf in 11150451. and the discovery of a potential companion ( 150.XU) in DD-04 4476. | The most positive results were the very faint detection of the cool white dwarf in HD150451 and the discovery of a potential companion $\sim 150$ AU) in BD-04 4476. |
More cata is required o draw any firm conclusions on the nature of these objects. | More data is required to draw any firm conclusions on the nature of these objects. |
Information regarding the current status of OSCA and instructions for observing with the svstem can be found on he ING website. | Information regarding the current status of OSCA and instructions for observing with the system can be found on the ING website. |
In memory of Richarcl Bingham. who passed away during the publication of this paper. | In memory of Richard Bingham, who passed away during the publication of this paper. |
Richarcl was a great colleague ancl a brilliant optical designer ancl will be sadly missed by us all. | Richard was a great colleague and a brilliant optical designer and will be sadly missed by us all. |
We would like to thank the Isaac Newton Group at he William Llerschel Telescope for their support during the comnmnissioning of OSCA. | We would like to thank the Isaac Newton Group at the William Herschel Telescope for their support during the commissioning of OSCA. |
We also thank the astronomers ab University College London and elsewhere that gave us wlp ancl suggestions for observing and objects of scientific interest. | We also thank the astronomers at University College London and elsewhere that gave us help and suggestions for observing and objects of scientific interest. |
The funding for OSCA was. provided. by the ἐν Particle Physies and Astronomy Research Council (PPARC). | The funding for OSCA was provided by the UK Particle Physics and Astronomy Research Council (PPARC). |
SJR acknowledges PPARC for. providing. the 1 | SJT acknowledges PPARC for providing the Ph. |
) studentship. during which the research for this paper was completed. | D studentship, during which the research for this paper was completed. |
‘This research. has made use of the SIAIBAD database. operated at CDS. Strasbourg. France | This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France |
of ? differs significantly by presenting a much higher fraction of very fast novae than the M31 data. | of \cite{2010AJ....140...34S} differs significantly by presenting a much higher fraction of very fast novae than the M31 data. |
For a fair comparison, one would have to correct the ? sample for its severe observational selection effects as being observed from inside the (dusty) Milky Way disk. | For a fair comparison, one would have to correct the \cite{2010AJ....140...34S} sample for its severe observational selection effects as being observed from inside the (dusty) Milky Way disk. |
A more detailed comparison is beyond the scope of this paper as it requires detailed modeling of the distribution of stellar and dust population of both galaxies. | A more detailed comparison is beyond the scope of this paper as it requires detailed modeling of the distribution of stellar and dust population of both galaxies. |
We have presented the position, outburst time and the maximum brightness of the 91 nova candidates discovered during the time span of the WeCAPP project. | We have presented the position, outburst time and the maximum brightness of the 91 nova candidates discovered during the time span of the WeCAPP project. |
Light-curve classifications under the taxonomic scheme of ? have been shown and the full and J--band light curves of each individual nova during the outburst are also presented in the Appendix. | Light-curve classifications under the taxonomic scheme of \cite{2010AJ....140...34S} have been shown and the full and -band light curves of each individual nova during the outburst are also presented in the Appendix. |
In this work we successfully applied a scheme developed for a Milky Way nova sample which, because of observational selection effects, is certainly dominated by the galactic disk, to a nova sample of a different host galaxy which is mostly observed towards the bulge of this host. | In this work we successfully applied a scheme developed for a Milky Way nova sample which, because of observational selection effects, is certainly dominated by the galactic disk, to a nova sample of a different host galaxy which is mostly observed towards the bulge of this host. |
The differences in member ratios for the subclasses as defined by ? between the Milky Way and our M31 WeCAPP sample probably reflect to some extent different observational selection effects, but bear the potential for further conclusions on the differences between stellar populations in M31 and the Milky Way, once the selection effects are proper accounted for. | The differences in member ratios for the subclasses as defined by \cite{2010AJ....140...34S} between the Milky Way and our M31 WeCAPP sample probably reflect to some extent different observational selection effects, but bear the potential for further conclusions on the differences between stellar populations in M31 and the Milky Way, once the selection effects are proper accounted for. |
We provide the full light curve data of the novae on request, as well as the postage stamps of the reduced, stacked, or difference-imaging frames. | We provide the full light curve data of the novae on request, as well as the postage stamps of the reduced, stacked, or difference-imaging frames. |
Part of this catalogue has been used to find the counter-part by ?? and showed that super soft X- sources (SSS) in M31 are mostly constituted by the novae during eruption. | Part of this catalogue has been used to find the X-ray counter-part by \cite{2005A+A...442..879P, 2007A+A...465..375P} and showed that super soft X-ray sources (SSS) in M31 are mostly constituted by the novae during eruption. |
The turn on and turn off of the SSS phase provide us the information of the ejected and accreted mass onto the surface of the white dwarf. | The turn on and turn off of the SSS phase provide us the information of the ejected and accreted mass onto the surface of the white dwarf. |
Besides the X-ray monitoring campaign, there is also a survey of M31 novae in infrared using (?),, which indicates a correlation between the dust formation timescales and the nova speed class. | Besides the X-ray monitoring campaign, there is also a survey of M31 novae in infrared using \citep{2011ApJ...727...50S}, which indicates a correlation between the dust formation timescales and the nova speed class. |
Such studies would not be possible without the speed class determined by the optical observations. | Such studies would not be possible without the speed class determined by the optical observations. |
Ground-based optical surveys, such as PTF (??),, PanSTARRS (7) and LSST (?),, will continue to play an important role in the regime of multi-wavelength novae observation and help us to gain insight of the underlying physical mechanism of novae. | Ground-based optical surveys, such as PTF \citep{2009PASP..121.1395L,2009PASP..121.1334R}, PanSTARRS \citep{2002SPIE.4836..154K} and LSST \citep{2002SPIE.4836...10T}, will continue to play an important role in the regime of multi-wavelength novae observation and help us to gain insight of the underlying physical mechanism of novae. |
regions are siiall aud could be unresolved sources. | regions are small and could be unresolved sources. |
Some of the diffuse emission uüght be iustriuuceuta because the point spread function of the NRT has a broad wing. | Some of the diffuse emission might be instrumental because the point spread function of the XRT has a broad wing. |
Excluding emission at the edee of the feld. we identify three sources. | Excluding emission at the edge of the field, we identify three sources. |
Two of them (UNL and ΠΝ2) ave somewhat exteuded aud might have more than one component: in ITXI. there appears to be a structure to the southeas of the amaxinaun. while IIN2S appears double. | Two of them (HX1 and HX3) are somewhat extended and might have more than one component; in HX1, there appears to be a structure to the southeast of the maximum, while HX3 appears double. |
Sources ITN? aud TENS are located close to regious NS and XN. respectively. aud. the deformation of the contours in Figure 2b corresponds to these hard sources. | Sources HX2 and HX3 are located close to regions XS and XN, respectively, and the deformation of the contours in Figure 2b corresponds to these hard sources. |
Table 1 sununarizes source properties. | Table 1 summarizes source properties. |
TIXN3-cast aud ΤΝποτ represent the cast and west componcuts of 180. respectively. | HX3-east and HX3-west represent the east and west components of HX3, respectively. |
The peak positious aud count rates are derived from Figure 2c. | The peak positions and count rates are derived from Figure 2c. |
The positioual uucertaiuty is ~1. | The positional uncertainty is $\sim 1'$. |
The count rates are uncertain < 20%) because of background subtraction. confusion with other sources. and the vignetting correction. | The count rates are uncertain $\simgt 20\%$ ) because of background subtraction, confusion with other sources, and the vignetting correction. |
The last four columns sunuuarize the properties of the radio counterparts (see 23.2 J. | The last four columns summarize the properties of the radio counterparts (see 3.2 ). |
Figure 2d is an X-ray color map generated from three enuergv bands: 0.71.5 keV (red). 1.52.5 keV (οπου). aud 2.56.0 keV (blue). aud offers an alternate wav to look at this region. | Figure 2d is an X-ray color map generated from three energy bands: 0.7–1.5 keV (red), 1.5–2.5 keV (green), and 2.5–6.0 keV (blue), and offers an alternate way to look at this region. |
The soft sources in Figure 2b appear with different colors. regions NN aud NS in vellow. region NW in ercen. and the faint features m the southeast in red. | The soft sources in Figure 2b appear with different colors, regions XN and XS in yellow, region XW in green, and the faint features in the southeast in red. |
This illustrates the result of NSS who found that the X-ray spectruii between 0.6 keV. and 2.2 keV beconies svstenmiaticallv harder toward the west. | This illustrates the result of KKS who found that the X-ray spectrum between 0.6 keV and 2.2 keV becomes systematically harder toward the west. |
As will be shown in 3.3. this is probably due to the absorption of intervening mterstellar eas. | As will be shown in 3.3, this is probably due to the absorption of intervening interstellar gas. |
The hard X-ray sources of Figure 2c appear blue in Figure 2d. | The hard X-ray sources of Figure 2c appear blue in Figure 2d. |
Figures 3a aud 3b are the soft aud lard SIS nuages of the central region of W51 (cf. | Figures 3a and 3b are the soft and hard SIS images of the central region of W51 (cf. |
Fig. | Fig. |
1). | 1). |
These have higher (~ 1) vesolutiou aud slow wore structure. | These have higher $\sim 1'$ ) resolution and show more structure. |
In order to help compare Figures 2 aud 3. we mark the peak positious iu Figures 2b aud 2c ax crosses In Fieures 3a and 3b. respectively. | In order to help compare Figures 2 and 3, we mark the peak positions in Figures 2b and 2c as crosses in Figures 3a and 3b, respectively. |
AccordingOo to FieureOo 3a. the brightestOo part of region NN is clongated (~ 23) eastwest. while the brightest part of region NS is resolved into northern and southern components. | According to Figure 3a, the brightest part of region XN is elongated $\sim 3'$ ) eastwest, while the brightest part of region XS is resolved into northern and southern components. |
In Figure 2b. TIX? is visible iu the southern area while IIN3-cast is barely visible near the northwestern boundary. | In Figure 3b, HX2 is visible in the southern area while HX3-east is barely visible near the northwestern boundary. |
IIN2 aud the southeru component of NS are both elongated castwest aud partly overlap. which suggests that they night be the same source. | HX2 and the southern component of XS are both elongated eastwest and partly overlap, which suggests that they might be the same source. |
An overlay of ταν and radio images helps to uuderstand this couples, region. | An overlay of X-ray and radio images helps to understand this complex region. |
Figure la compares the ROSAT X-rav image of IKKS with a radio contour map. | Figure 4a compares the ROSAT X-ray image of KKS with a radio contour map. |
This ROSAT image contains almost the same information as the soft A-rav nap but covers a larecr area. | This ROSAT image contains almost the same information as the soft X-ray map but covers a larger area. |
KEKS did a Ιλία comparison. but the radio maps that they used either lac poor angular resolution 1.2) or did not show large-scale Z15") structures. | KKS did a similar comparison, but the radio maps that they used either had poor angular resolution $4.'2$ ) or did not show large-scale $\simgt 15'$ ) structures. |
Figure la uses the 330 MITZz map of Subralimiauva&Coss(1995) which shows the detailed (~1) structures over the whole couples. | Figure 4a uses the 330 MHz map of \citet{sub95} which shows the detailed $\sim 1'$ ) structures over the whole complex. |
Iu Figure la. the clusters of comipact sources in the rorth aud near the ceuter are known as the W51À and W51D II II reeion complexes. respectively. | In Figure 4a, the clusters of compact sources in the north and near the center are known as the W51A and W51B H II region complexes, respectively. |
The W51C SNR appears as au incomplete. very hick radio shell iu the southeast. | The W51C SNR appears as an incomplete, very thick radio shell in the southeast. |
The caster X-rav shell matches alinost perfectly with the outer )oundary as expected for à SNR. | The eastern X-ray shell matches almost perfectly with the outer boundary as expected for a SNR. |
Reeious NN aud NS are partly surrounded by the radio shell. aud hey appear to be immersed in a diffuse N-rav enüssiou together with the eastern XN-rav shell. | Regions XN and XS are partly surrounded by the radio shell, and they appear to be immersed in a diffuse X-ray emission together with the eastern X-ray shell. |
This müeht indicate that they are parts of the SNR too. | This might indicate that they are parts of the SNR too. |
SNRs with ceutrally-brightcned N-rav Cluission are not unusual (see 5.1). | SNRs with centrally-brightened X-ray emission are not unusual (see 5.1). |
On the other haud. the western half of the SNR is uot clearly defined in radio because of the superimposed source W51D. But the western edge of the radio source is also iuatehed ta XN-rav cussion with region NW. | On the other hand, the western half of the SNR is not clearly defined in radio because of the superimposed source W51B. But the western edge of the radio source is also matched in X-ray emission with region XW. |
This probably shows the western shell ofthe SNR. | This probably shows the western shell of the SNR. |
Iu L1. we will show that reeious NN. XS. aud NW are all located at the far-side of the Sagittarius aru and have similar tempcratures. which sugeests that they are all possibly parts of a single SNR. | In 4.1, we will show that regions XN, XS, and XW are all located at the far-side of the Sagittarius arm and have similar temperatures, which suggests that they are all possibly parts of a single SNR. |
Figure Ib compares the hard X-ray image with the radio nuage aud shows that some of the lard A-rav sources are associated with compact radio sources, | Figure 4b compares the hard X-ray image with the radio image and shows that some of the hard X-ray sources are associated with compact radio sources. |
First. ITNT coincides with 0.3 and 0.3 which are compact I IT regious. | First, HX1 coincides with $-$ 0.3 and $-$ 0.3 which are compact H II regions. |
Secoud. IIX3-east. coincides with 0.3. also a compact IT IT region. | Second, HX3-east coincides with $-$ 0.3, also a compact H II region. |
Third. the bright ταν source at the northeru boundary of the field nmüeht be associated with W5SLA which is mostly outside the field of view. | Third, the bright X-ray source at the northern boundary of the field might be associated with W51A which is mostly outside the field of view. |
The hard | The hard |
spectrograph fiber would. sample systematically clilferent physical radii in galaxies observed: under dillerent angles. | spectrograph fiber would sample systematically different physical radii in galaxies observed under different angles. |
We show the Sersic index distributions of quiescent ellipticals. quiescent spirals and. all the spirals in our catalog. selected by a cdebiased probability Posic00.5 of having the respective morphological ἵνρο in Fig. 4.. | We show the Sersic index distributions of quiescent ellipticals, quiescent spirals and all the spirals in our catalog, selected by a debiased probability $P_{debiased}>0.8$ of having the respective morphological type in Fig. \ref{fig:sersic}. |
Notably. quiescent spiral galaxies present a cillerent Sersic distribution than star-forming spiral galaxies —dominated by blue disks. peaking at ηx4 instead. of lower value of nol.52 of blue spirals. | Notably, quiescent spiral galaxies present a different Sersic distribution than star-forming spiral galaxies –dominated by blue disks–, peaking at $n\simeq 4$ instead of lower value of $n\sim 1.5-2$ of blue spirals. |
This is indicative of the presence of large bulges in these objects. | This is indicative of the presence of large bulges in these objects. |
We note that introducing a further cut in p to select elliptical galaxies (i. ο. selecting only elliptical galaxies with η= 3) makes no dillerence to our final results. | We note that introducing a further cut in $n$ to select elliptical galaxies (i. e., selecting only elliptical galaxies with $n>3$ ) makes no difference to our final results. |
Ideally. we would compare the stellar populations in thebudges of spiral and elliptical galaxies. as in the works by Proctor&Sansom(2002):ThomasDavies(2006).. bu eiven the degencracy between bulge-to-total ratio (B/T). physical size ancl angular distance evolution and the fixe size of the SDSS specrograph fibre we will be probing the stellar populations in theregions. that are indeec dominated by the bulge. | Ideally, we would compare the stellar populations in the of spiral and elliptical galaxies, as in the works by \citet{proctor02, thomas06}, but given the degeneracy between bulge-to-total ratio (B/T), physical size and angular distance evolution and the fixed size of the SDSS spectrograph fibre we will be probing the stellar populations in the, that are indeed dominated by the bulge. |
Given the typical high sersie index of quiescent spirals. itis very likely that the light within £2, is dominated by a prominent bulge. | Given the typical high sersic index of quiescent spirals, it is very likely that the light within $R_e$ is dominated by a prominent bulge. |
Nonetheless. we can no discard. some contribution from stellar populations in the inner disk. although we deem it to be a second-order eflec since we specifically select. galaxies with quiescent: stellar populationsover the galaxy. | Nonetheless, we can not discard some contribution from stellar populations in the inner disk, although we deem it to be a second-order effect since we specifically select galaxies with quiescent stellar populations the galaxy. |
We will also test our main results for a subsample of galaxies for which we know the light in the fiber to be bulge-dominated. | We will also test our main results for a subsample of galaxies for which we know the light in the fiber to be bulge-dominated. |
While we focus in the comparison between elliptical and face-on spiral galaxies. we will also show in some of our plots a third. group of galaxies. composed. of edge-on. quiescent disks selected from the NYU-VAC to have b/a«0.4. and no constraint in GZ visual classification. | While we focus in the comparison between elliptical and face-on spiral galaxies, we will also show in some of our plots a third group of galaxies, composed of edge-on quiescent disks selected from the NYU-VAC to have $b/a<0.4$ –and no constraint in GZ visual classification. |
When comparing this with the two aforementioned. samples (edge- and face-on quiescent disks). the reader should bear in mind that in many cases the amount of light originated by the disks? stellar populations in edge-on objects will be larger than in the case of the GZ ace-on quiescent spiral sample. | When comparing this with the two aforementioned samples (edge- and face-on quiescent disks), the reader should bear in mind that in many cases the amount of light originated by the disks' stellar populations in edge-on objects will be larger than in the case of the GZ face-on quiescent spiral sample. |
As a summary of our sample selection. we use SDSS DIU galaxies at 0.04<20.1 with logMfM.>10.4. | As a summary of our sample selection, we use SDSS DR7 galaxies at $0.04<z<0.1$ with $log M_*/M_\odot > 10.4$. |
Objects are selected to show optical ηr color compatible with red sequence galaxies. no ££, emission in the spectra. | Objects are selected to show optical $u-r$ color compatible with red sequence galaxies, no $H_\alpha$ emission in the spectra. |
Additionally we select them photometrically to be quiescent inthe sw rysrz diagram following Williamsetal.(2009) and. Holdenetal.(20101). | Additionally we select them photometrically to be quiescent in the $u-r$ vs $r-z$ diagram following \citet{williams} and \citet{holden11}. |
.. AL objects must have debiased probability P?0.8 of being either spiral or elliptical in the Galaxy Zoo catalog. | All objects must have debiased probability $P > 0.8$ of being either spiral or elliptical in the Galaxy Zoo catalog. |
Furthermore. we include only those spiral galaxies with low cllipticity (b/a> 0.5). | Furthermore, we include only those spiral galaxies with low ellipticity $b/a>0.5$ ). |
We will show [or comparison purposes edge-on quiescent disk galaxies selected from the NYU-VAC to have b/a«0.4. | We will show for comparison purposes edge-on quiescent disk galaxies selected from the NYU-VAC to have $b/a <0.4$. |
This leaves us with a sample of approximately 14700 early tvpe galaxies ancl 1000 face-on spirals. | This leaves us with a sample of approximately 14700 early type galaxies and 1000 face-on spirals. |
In this paper. we perform adifferential analysis of the stellar populations in the central regions of quiescent spiral and elliptical galaxies. | In this paper, we perform a analysis of the stellar populations in the central regions of quiescent spiral and elliptical galaxies. |
We compare. in particular. the metallicity. a enhancement (traced by the excess of ο) and r-band light-weightec age of those two groups of galaxies over the redshift range 0.04<z0.1 and with stellar. masses log(AL,AM.)z10.4. | We compare, in particular, the metallicity, $\alpha-$ enhancement (traced by the excess of $\langle$ $\rangle$ ) and r-band light-weighted age of those two groups of galaxies over the redshift range $0.04<z<0.1$ and with stellar masses $(M_*/M_\odot)>10.4$. |
In Fig. | In Fig. |
5 we show the median values of those quantities in bins of stellar mass. | \ref{fig:vsmass} we show the median values of those quantities in bins of stellar mass. |
The metallicity in all three sub-samples is remarkably similar over the whole mass range explored in this paper. | The metallicity in all three sub-samples is remarkably similar over the whole mass range explored in this paper. |
“Phey are not only compatible within the la typical dispersion. shown as the large error bar on the right side of the plot. but also the position of the mean of both distributions are indistinguishable. | They are not only compatible within the $1 \sigma$ typical dispersion, shown as the large error bar on the right side of the plot, but also the position of the mean of both distributions are indistinguishable. |
Phe error in the position of the mean is denoted by the error in every. mass bin. | The error in the position of the mean is denoted by the error in every mass bin. |
due to the second part of D... is Chen obtained by using the same procedure. wilh ó replaced bv —6ó. | due to the second part of $D_\pm$, is then obtained by using the same procedure, with $\phi$ replaced by $-\phi$. |
The last step is onlycarried out when ὦ<15: otherwise. positrons are ignored. | The last step is onlycarried out when $\phi<15$; otherwise, positrons are ignored. |
The pressure ionization term in (he free energy is (taken from ?:: where the 13.60 is in eV. and the units of οι and e; are . | The pressure ionization term in the free energy is taken from \citet{1995MNRAS.274..964P}: where the 13.60 is in eV, and the units of $c_1$ and $c_4$ are $^{-3}$. |
Furthermore. iy is the total number of electrons. bound or Iree. and neg=Noo/V. | Furthermore, $N_{e0}$ is the total number of electrons, bound or free, and $n_{e0}=N_{e0}/V$. |
The object of Fp; is to induce pressure ionization by reducing the electronic chemical potential as (he number of electrons n.a) in a cube with side αμ. the Dohr radius. increases. | The object of $F_{PI}$ is to induce pressure ionization by reducing the electronic chemical potential as the number of electrons $n_ea_0^3$ in a cube with side $a_0$, the Bohr radius, increases. |
Of course Fp, tends to zero as lonizalion becomes complete. that is. as IN.—Ny. | Of course $F_{PI}$ tends to zero as ionization becomes complete, that is, as $N_e\rightarrow N_{e0}$. |
The last term. Fe. in the [ree energy depends on the Coulomb parameter P and on the Debve parameter A. | The last term, $F_{CQ}$, in the free energy depends on the Coulomb parameter $\Gamma$ and on the Debye parameter $\Lambda$. |
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