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This model can predict the evolution of the abundances of 37 chemical elements from the light to the heavy ones. | This model can predict the evolution of the abundances of 37 chemical elements from the light to the heavy ones. |
We use this nodel to reproduce the chemical evolution of the Milky Way disk and that of the two nearby spiral galaxies (M31 and M33). | We use this model to reproduce the chemical evolution of the Milky Way disk and that of the two nearby spiral galaxies (M31 and M33). |
To do that. we assume that the disk of each galaxy formed by gas aceretion and vary the star formation efficiency as well as the gas accretion timescale. | To do that, we assume that the disk of each galaxy formed by gas accretion and vary the star formation efficiency as well as the gas accretion timescale. |
The similarities and the differences between the chemical evolution of these objects and the Milky Way are discussed to provide a basis for the understanding of the chemical evolution of disks. | The similarities and the differences between the chemical evolution of these objects and the Milky Way are discussed to provide a basis for the understanding of the chemical evolution of disks. |
The paper is organized as follows: in section 2 we describe our chemical evolution model and the assumptions made for each galaxy. | The paper is organized as follows: in section 2 we describe our chemical evolution model and the assumptions made for each galaxy. |
In section 3 we present the results for the models and these results are discussed in detail in section 4. | In section 3 we present the results for the models and these results are discussed in detail in section 4. |
Finally in section 5 we summarize our conclusions. | Finally in section 5 we summarize our conclusions. |
the arctangent. Gt is useful to determine the amplitude of the RC. | the arctangent fit is useful to determine the amplitude of the RC. |
The general kinematical properties of the four. polar- candidates for which the velocity profiles were measured are summarized in Table 1.. | The general kinematical properties of the four polar-ring candidates for which the velocity profiles were measured are summarized in Table \ref{rc}. |
The second and third columns of Table 1 list the arctangent [it parameters Vinax Ando ory. | The second and third columns of Table \ref{rc} list the arctangent fit parameters $_{\rm max}$ and $r_t$. |
The fourth column gives the maximum. rotation velocity corrected for the inclination of the galaxy: Vineasxe=Vinex/si. where the inclination / is estimated from the apparent axial ratio. | The fourth column gives the maximum rotation velocity corrected for the inclination of the galaxy: $_{\rm
max,c}$ $_{\rm max}$ $i$, where the inclination $i$ is estimated from the apparent axial ratio. |
In the fifth. column we present optical radii of the galaxies (measured. from. the DSS images). and the sixth. column lists our estimate of the total galaxy mass within the optical radius under the assumption of a spherical mass clistribution. | In the fifth column we present optical radii of the galaxies (measured from the DSS images), and the sixth column lists our estimate of the total galaxy mass within the optical radius under the assumption of a spherical mass distribution. |
The Last. two columns contain the ratio of mass to observed. luminosity and the relative content. respectively. | The last two columns contain the ratio of mass to observed luminosity and the relative content, respectively. |
As can be seen from ‘Table 1.. polar-ring candidates show characteristics which are quite common for tvpical spiral galaxies (the comparatively large value of Απ ερ for AAL 1934-563 may. be partially explained by its almost cdge-on orientation: the magnitucle corrected to a face-on orientation may be as much as ~| brighter). | As can be seen from Table \ref{rc}, polar-ring candidates show characteristics which are quite common for typical spiral galaxies (the comparatively large value of $_{\rm tot}$ $L_B$ for AM 1934-563 may be partially explained by its almost edge-on orientation; the magnitude corrected to a face-on orientation may be as much as $\sim
1^{\rm m}$ brighter). |
In Fig. | In Fig. |
1 we compare the Tullv-Fisher relation for normal spiral galaxies (Brocils 1992) to that of our spiral polar-ring candidates. | \ref{tf} we compare the Tully-Fisher relation for normal spiral galaxies (Broeils 1992) to that of our spiral polar-ring candidates. |
For the latter we used. maximum. rotation velocities corrected. for inclination. ancl absolute Iuminosities (cle Vaucouleurs et al. | For the latter we used maximum rotation velocities corrected for inclination and absolute luminosities (de Vaucouleurs et al. |
1991). | 1991). |
As can be seen. two ealaxies (AAL 1934-563. and ESO 500-CG41) follow the relation for normal spirals. while two others (ESO 576-CG69 and AM. 1837-631). have too Large luminosities (for. fixed Vines) OF too small rotation velocities for their. Iuminosity. | As can be seen, two galaxies (AM 1934-563 and ESO 500-G41) follow the relation for normal spirals, while two others (ESO 576-G69 and AM 1837-631) have too large luminosities (for fixed $_{\rm max}$ ) or too small rotation velocities for their luminosity. |
-robably both of these possible reasons can contribute to he observed deviations. as galaxy interactions and mergers can enhance optical luminosities as well as disturb ine velocity fields in the involved. galaxies. | Probably both of these possible reasons can contribute to the observed deviations, as galaxy interactions and mergers can enhance optical luminosities as well as disturb emission-line velocity fields in the involved galaxies. |
In Fig. | In Fig. |
1 we plot the nuclear stellar velocity dispersion (7) and the nuclear linewidth (EWIIM) of. A6583. indicating the velocity dispersion of the interstellar gas. as à unction of the total blue absolute magnitude for the sample of elliptical and SO galaxies observed by Phillips et al. ( | \ref{2mb} we plot the nuclear stellar velocity dispersion $\sigma$ ) and the nuclear linewidth (FWHM) of $\lambda$ 6583, indicating the velocity dispersion of the interstellar gas, as a function of the total blue absolute magnitude for the sample of elliptical and S0 galaxies observed by Phillips et al. ( |
150) (redshifts. apparent magnitudes and velocity clispersions are aken from NED and LEDA databases) | 1986) (redshifts, apparent magnitudes and velocity dispersions are taken from NED and LEDA databases). |
As one can sec. the increase of the central velocity dispersion of the gas with AI(B) is similar to that observed for the stars. though with a larger dispersion and a notable svstematic shift. | As one can see, the increase of the central velocity dispersion of the gas with M(B) is similar to that observed for the stars, though with a larger dispersion and a notable systematic shift. |
Phe mean ratio of u]) to o is 2.080.124 (s.e.m.). | The mean ratio of ]) to $\sigma$ is $\pm$ 0.14 (s.e.m.). |
In Pig. | In Fig. |
1 the polar-ring galaxies ESO 503-CG17. NCC 5122. ESO G4 (present. paper). IC 1689 (Llagen- 1997).. ος 4323. and NGC 4753 (Reshetnikov&Combes19904) are located in the same region as normal early-type galaxies. | \ref{2mb} the polar-ring galaxies ESO 503-G17, NGC 5122, ESO 232-G4 (present paper), IC 1689 \cite{ht}, UGC 4323, and NGC 4753 \cite{rc} are located in the same region as normal early-type galaxies. |
The peculiar spiral galaxy ESO 576-G69 (C-46) is the most interesting object in our sample. | The peculiar spiral galaxy ESO 576-G69 (C-46) is the most interesting object in our sample. |
As shown by Carilli van Gorkom (1992). an asymmetric ring-like structure surrounding the galaxy along the minor axis (probably a polar ring) rotates around the major axis of ISO 576-G69 with Vis7100 km s.+. | As shown by Carilli van Gorkom (1992), an asymmetric ring-like structure surrounding the galaxy along the minor axis (probably a polar ring) rotates around the major axis of ESO 576-G69 with $_{\rm max}\sim$ 100 km $\rm s^{-1}$. |
Our kinematical observations show that the main body of the galaxy. on the other hand. rotates around the minor axis. | Our kinematical observations show that the main body of the galaxy, on the other hand, rotates around the minor axis. |
Pherefore. ESO 576-669 can be classified. as agalary. Vhis kind of extragalactic objects is extremely rare (e.g. VGC 4385. Reshetnikov Combes 1994. NGC 660 van Driel et al. | Therefore, ESO 576-G69 can be classified as a. This kind of extragalactic objects is extremely rare (e.g. UGC 4385 – Reshetnikov Combes 1994, NGC 660 – van Driel et al. |
1995). | 1995). |
Our results provide new data on nuclear properties of PRGs. | Our results provide new data on nuclear properties of PRGs. |
A first look at Table 1. shows that active nuclei are overpresented in the sample. where they represent 00 per cent (5/8). | A first look at Table \ref{charsum} shows that active nuclei are overpresented in the sample, where they represent $\sim$ 60 per cent (5/8). |
Because of the small sample size. this conclusion is not statistically significant. | Because of the small sample size, this conclusion is not statistically significant. |
However. considering all 16 objects from Reshetnikoy Combes (1094) às well as the cata on NGC 2685 (Willneretal.1985).. NGC 660 (vanDrieletal.1995).. and 1€ 1689. (Ilagen-Fhorn.&Reshetnikoy 1997).. the sample of PRs and candidates with nuclear spectra increases to 27 galaxies. | However, considering all 16 objects from Reshetnikov Combes \shortcite{rc} as well as the data on NGC 2685 \cite{wef}, NGC 660 \cite{van}, and IC 1689 \cite{ht}, the sample of PRGs and candidates with nuclear spectra increases to 27 galaxies. |
OL these at least 14 (52 per cent) have LINER. or Sevfert. nuclei. | Of these at least 14 (52 per cent) have LINER or Seyfert nuclei. |
Considered separately. and according to the original papers. Sevfert nuclei are. found. in 36 objects (the first. number refers to confident classifications and the second one includes uncertain classifications) or 12.525 per cent. respectively. and LINERs in a total of S11 objects (counted: as above) or 3341 per cent. | Considered separately, and according to the original papers, Seyfert nuclei are found in 3–6 objects (the first number refers to confident classifications and the second one includes uncertain classifications) or 12.5–25 per cent, respectively, and LINERs in a total of 8–11 objects (counted as above) or 33–41 per cent. |
Therefore. the fraction of active nuclei is high among PIs and candidates. | Therefore, the fraction of active nuclei is high among PRGs and candidates. |
PRGs hosting AGNs are predominantly SO galaxies. | PRGs hosting AGNs are predominantly S0 galaxies. |
It would be interesting to compare the number of SO...) and SU,Lixpns Co the number of ordinary SO. | It would be interesting to compare the number of $_{\rm(Sey)}$ and $_{\rm(LINERS)}$ to the number of ordinary S0. |
This requires good morphological classifications of our PCs and. candidates. but such comparison is presently impossible since the available data is neither good. nor abundant enough for the classification. | This requires good morphological classifications of our PRGs and candidates, but such comparison is presently impossible since the available data is neither good nor abundant enough for the classification. |
Moreover. most PRC candidates are very peculiar and faint. | Moreover, most PRG candidates are very peculiar and faint. |
More detailed ancl precise statistics can only be done when we have a sample of PRGs at least twice as large as presently available together with good optical images. | More detailed and precise statistics can only be done when we have a sample of PRGs at least twice as large as presently available together with good optical images. |
PRGs are very heterogeneous objects regarding both morphology and environment. | PRGs are very heterogeneous objects regarding both morphology and environment. |
However. they have one particular. feature. in) common: the existence of two large-scale. stronely inclined kinematic subsystems. | However, they have one particular feature in common: the existence of two large-scale strongly inclined kinematic subsystems. |
Such complicated. internal kinematics are considered: usually as a consequence of relatively long-lasting galaxy interactions. accompanied by mass transfer from one galaxy to another (ranging from. eas accretion to complete merging). | Such complicated internal kinematics are considered usually as a consequence of relatively long-lasting galaxy interactions, accompanied by mass transfer from one galaxy to another (ranging from gas accretion to complete merging). |
One can speculate that such interactions are favourable for the formation of non-thermal nuclear activity. | One can speculate that such interactions are favourable for the formation of non-thermal nuclear activity. |
Due to the limited size of our sample this conclusion must. however. remain tentative for the time being. | Due to the limited size of our sample this conclusion must, however, remain tentative for the time being. |
Changes the counts iu cells distribution slightly from the siugle-species result. given by equation (1)). | changes the counts in cells distribution slightly from the single-species result given by equation \ref{eint-GQED}) ). |
As a result of mergers. the clustering parameter 6 increases with time. and we have shown that it depeuds very weakly ou the physical extent of a galaxy and the seale Ay at which the two point correlation function is negligible. | As a result of mergers, the clustering parameter $b$ increases with time, and we have shown that it depends very weakly on the physical extent of a galaxy and the scale $R_1$ at which the two point correlation function is negligible. |
The effect of the physical extent of a galaxy ehauges db/dz by less han2%... which shows that the evolution of 6 depends mainly on the adiabatic expansion of the universe aud the change in the number of galaxies from mergers. | The effect of the physical extent of a galaxy changes $db/dz$ by less than, which shows that the evolution of $b$ depends mainly on the adiabatic expansion of the universe and the change in the number of galaxies from mergers. |
These results show the even when we take galaxy mergers iuto account. we can not only 'eproduce the GQED but also trace the evolution of tle clustering parameters. | These results show that even when we take galaxy mergers into account, we can not only reproduce the GQED but also trace the evolution of the clustering parameters. |
However. au analysis of the GOODS catalog (2)— iudicates a large variation between the North aud South fields aud suggests that the sample is probably too πια to draw. any imeaniugful couclusious about the evolution of b at high redshilt. | However, an analysis of the GOODS catalog \citep{2009ApJ...695.1121R}
indicates a large variation between the North and South fields and suggests that the sample is probably too small to draw any meaningful conclusions about the evolution of $b$ at high redshift. |
Future surveys however may provide sullicieutly large samples at high redshilts to test our predicted evolution of b. | Future surveys however may provide sufficiently large samples at high redshifts to test our predicted evolution of $b$. |
A. Yang is grateful for the support from the National University of Singapore and the Institute of Astronomy of the University of Cambridee where part of this work was clone. | A. Yang is grateful for the support from the National University of Singapore and the Institute of Astronomy of the University of Cambridge where part of this work was done. |
A. H. Chan would like to thank the departinent of History Philosophy of Science. Cambridge University aud Nanyaug Polytechnic for kind hospitality where part of the initial work was clone. | A. H. Chan would like to thank the department of History Philosophy of Science, Cambridge University and Nanyang Polytechnic for kind hospitality where part of the initial work was done. |
Chandra observatories, | Chandra observatories. |
As results inferred from differcut iustruineuts are subject to calibration uncertainties (sec. e. ον Durwitz et al. | As results inferred from different instruments are subject to calibration uncertainties (see, e. g., Burwitz et al. |
2001. for the case of 3750). we used only the Chandra data collected with the LETCS erating instrument iu a total exposure of 37.5 ks in February 2000. | \cite{burwitz03} for the case of ), we used only the Chandra data collected with the LETGS grating instrument in a total exposure of 37.5 ks in February 2000. |
First results from the spectral analysis of these data have been preseuted i Pavlov et al. (2002)). | First results from the spectral analysis of these data have been presented in Pavlov et al. \cite{pavlov2002}) ). |
They found that ucither light-clement (livdrogen or heliuui) nor heavy-cleimeut (pure irou or solar mixture} jieutron star atimosphere models cau explain the nulti-wavelength spectral distribution of the euission detectec ToniJ0720. | They found that neither light-element (hydrogen or helium) nor heavy-element (pure iron or solar mixture) neutron star atmosphere models can explain the multi-wavelength spectral distribution of the emission detected from. |
1-3125.. The uct result of this analysis was remarkably similar to the situation with the spectra fitting of the optical and A-rav data ou1: while providing acceptable fits to the N-rav data the light-clement atmosphere models vield wurealistic large radii of he INS and significantly wer-prediet the actual optica fluxes (by a factor of ~ 300). whereas the heavy-cleme nodels do not fit the N-ray data due to nuuerous features in the model spectra caused by absorption at atomic ranitious in ious of the heavy elemieuts (see Zavliu Pavlov 2002. for details). | The net result of this analysis was remarkably similar to the situation with the spectral fitting of the optical and X-ray data on: while providing acceptable fits to the X-ray data the light-element atmosphere models yield unrealistic large radii of the INS and significantly over-predict the actual optical fluxes (by a factor of $\sim 300$ ), whereas the heavy-element models do not fit the X-ray data due to numerous features in the model spectra caused by absorption at atomic transitions in ions of the heavy elements (see Zavlin Pavlov \cite{zavlin02} for details). |
Pavlov et al. (20023) | Pavlov et al. \cite{pavlov2002}) ) |
found that he best fit to the Chaudra LETCS data ou lis provided by a blackbody model with the temperature «Τῃ,=80082 eV cuutted from am area of a radius Ro=(2.02.2)(D/L00pe) kan (D is the distance to he source). absorbed with the bydrogen column density Ny=tl.»yo17)x1079JD D3. | found that the best fit to the Chandra LETGS data on is provided by a blackbody model with the temperature $^\infty_{\rm bb}=80-82$ eV emitted from an area of a radius $^\infty_{\rm
bb}=(2.0-2.2)\,({\rm D}/100\,{\rm pc})$ km (D is the distance to the source), absorbed with the hydrogen column density $_{\rm H}=(1.5-1.7)\times 10^{20}$ $^{-2}$. |
Similar to the case ofJLS56.5-3751... the best Dlackhody model derived from the N-rav data on munderpredicts the optical fluxes detected from the source by a factor of [. | Similar to the case of, the best blackbody model derived from the X-ray data on underpredicts the optical fluxes detected from the source by a factor of 4. |
Paxων et al. (2002)) | Pavlov et al. \cite{pavlov2002}) ) |
speculated that a two-blackbody imodel. originally sugeested bv Pons et al. (2002)) | speculated that a two-blackbody model, originally suggested by Pons et al. \cite{pons02}) ) |
to descvibe the multiwaveleugth data on L.. uav be also applied to the radiation fronJ0720.1-3125... with the "soft conipoueut of kT.DENS< ον and Bj.DENS>6.1(D/100pc] kii. | to describe the multi-wavelength data on , may be also applied to the radiation from, with the “soft” component of $^\infty_{\rm bb,s}<43$ eV and $^\infty_{\rm bb,s}>6.1\,({\rm D}/100\,{\rm pc})$ km. |
Such a model. with N-vavs originating from a hot area on the stars surface and the optical fluxes emütted from the rest of the surface. 1nay explain the pulsatious of the N-vay radiation frouJo720.1-3125.. | Such a model, with X-rays originating from a hot area on the star's surface and the optical fluxes emitted from the rest of the surface, may explain the pulsations of the X-ray radiation from. |
In addition to the thermal componoetits. HIST. observations bv Kaplan ο al. (2003)) | In addition to the thermal components, HST observations by Kaplan et al. \cite{kaplan03}) ) |
reveal evidence for a uouthermal power law colpoucut. | reveal evidence for a nonthermal power law component. |
Towever. while tlis siniple iiultiple-coniponenut mode seclus to be idu agreement with the properties of the ciission detected fromJ0720.1-3125... it. ds hardly reconciled with the fact that. as stars are uot blackbodies. raclation enütted by a star shouk deviate from a blacAbodyv model. | However, while this simple multiple-component model seems to be in agreement with the properties of the emission detected from, it is hardly reconciled with the fact that, as stars are not blackbodies, radiation emitted by a star should deviate from a blackbody model. |
Also. i the case ofRXJ1556.5-375L. the absence of pulsatious put severe constraluts on he two-blackbody model. requiring either a particular ecometrical coufiguration or strong eravitational detlectio1 (Ransom et al. 2002)). | Also, in the case of, the absence of pulsations put severe constraints on the two-blackbody model, requiring either a particular geometrical configuration or strong gravitational deflection (Ransom et al. \cite{ransom02}) ). |
All previous modes of neutron star surface radiation were based on a conventional assmuption that there is chough matter ο, BS.ο nue liverogon or iron. or a müxture of clemeuts) ou the icutron star surface to make the atmosphere lavers optically thick at all euergies of interest. | All previous models of neutron star surface radiation were based on a conventional assumption that there is enough matter (e. g., pure hydrogen or iron, or a mixture of elements) on the neutron star surface to make the atmosphere layers optically thick at all energies of interest. |
A typical estimate for such au amount in terms of the total surface. column deusitv+ is. và;7+10—E100 & P= (depending ou the surface temperature) to provide the equilibrium (or diffusima) solution of the radiative transfer problein in the very cep lavers (see AMihalas 1978)). | A typical estimate for such an amount in terms of the total surface column density is $_{\rm
tot}>10-100$ g $^{-2}$ (depending on the surface temperature) to provide the equilibrium (or diffusion) solution of the radiative transfer problem in the very deep layers (see Mihalas \cite{mihalas78}) ). |
Under this assuniption. spectra of the emitted radiation are solely determined by the temperature distribution in the atinosphere (Gvehich grows towards larger depths) and do uot depend «n properties of stars lavers ling uuderneath the atmosphere. | Under this assumption, spectra of the emitted radiation are solely determined by the temperature distribution in the atmosphere (which grows towards larger depths) and do not depend on properties of star's layers lying underneath the atmosphere. |
In the case of a lieht-clement atmosphere composition. the model spectra were ound to be much larder at higherLad photon energies than dackbody. ones providing the same radiative fux. | In the case of a light-element atmosphere composition, the model spectra were found to be much harder at higher photon energies than blackbody ones providing the same radiative flux. |
The reason. for this effect is that ligh-enerey photons with οσο mean-frec-patlis are ciitted from deep surface avers with temperatures larger than the so-called effective eniperature. the fourth power of which determines the otal enerev fux (x cae. Zavliu ct al. | The reason for this effect is that high-energy photons with longer mean-free-paths are emitted from deep surface layers with temperatures larger than the so-called effective temperature, the fourth power of which determines the total energy flux (see, e.g., Zavlin et al. |
1996. aud Zavlin Pavlov 2002 for details}. | \cite{zavlin96} and Zavlin Pavlov \cite{zavlin02} for details). |
Due to this property he model spectra. wwhen applied to observational data. usually vield lower toiuperatures by a factor of 2.3 and uuch larger enüttius areas by afactor of 50200 than estimates obtained froni blackbody fits. | Due to this property the model spectra, when applied to observational data, usually yield lower temperatures by a factor of $2-3$ and much larger emitting areas by afactor of $50-200$ than estimates obtained from blackbody fits. |
IHowever. it is iof known a priori how mich. for example. hydrogen las | However, it is not known a priori how much, for example, hydrogen has |
To approximate the probability of a chance superposition of the X-ray positions of the compact sources with random sources in the respective fields. we calculate P=|expeve '* where pa is the surface area number density of observed sources down to the limiting magnitude and Ar, is the area of the X-ray positional error. | To approximate the probability of a chance superposition of the X-ray positions of the compact sources with random sources in the respective fields, we calculate $P \approx 1-\exp^{-(\rho_N \times A_{Err})}$ ; where $\rho_N$ is the surface area number density of observed sources down to the limiting magnitude and $A_{Err}$ is the area of the X-ray positional error. |
For aandJ18490—0000.. which have positions accurate at the sub-aresecond level. we find probabilities of chance superpositions of and respectively. making the positional coincidence of wwith a nIR object reasonably compelling evidence for its association. | For and, which have positions accurate at the sub-arcsecond level, we find probabilities of chance superpositions of and respectively, making the positional coincidence of with a nIR object reasonably compelling evidence for its association. |
However. forJ1632—478.. with only an aresecond accurate position. the probability is much greater at50%.. though the source is in a relatively less densely populated region of the field. where the local probability is ~40%. | However, for, with only an arcsecond accurate position, the probability is much greater at, though the source is in a relatively less densely populated region of the field, where the local probability is $\sim 40\%$. |
In this case. even if a source had been found within the error circle. its associatiol with the X-ray source would be weak. meaning source | at a distance of ~2.60 is likely unrelated. | In this case, even if a source had been found within the error circle, its association with the X-ray source would be weak, meaning source 1 at a distance of $\sim 2.6\sigma$ is likely unrelated. |
To associate a nIR counterpart with this source based on positional coincidence will require a significantly. better constrained position from e.g.Chandra. Along with the optical extinction in their directions. the detection of extended emission from the PWNe is complicated by the high level of background in nIR observations as well as the generally high density of field sources in the Galactic plane which contaminate the background. | To associate a nIR counterpart with this source based on positional coincidence will require a significantly better constrained position from e.g. Along with the optical extinction in their directions, the detection of extended emission from the PWNe is complicated by the high level of background in nIR observations as well as the generally high density of field sources in the Galactic plane which contaminate the background. |
Deep nIR images from larger telescopes better able to resolve field sources. may be able to detect PWN emission. as well as increasing the probability of detecting the compact sources. but in these directions source confusion will always be a major impediment to detection of point or extended sources. | Deep nIR images from larger telescopes better able to resolve field sources, may be able to detect PWN emission, as well as increasing the probability of detecting the compact sources, but in these directions source confusion will always be a major impediment to detection of point or extended sources. |
We find no evidence of any extended nIR emission associated with the PWNe in any of the fields or any new counterparts to the X-ray point sources. but we do confirm the magnitude of the previously suggested counterpart. ofJ18490—0000. | We find no evidence of any extended nIR emission associated with the PWNe in any of the fields or any new counterparts to the X-ray point sources, but we do confirm the magnitude of the previously suggested counterpart of. |
. While there is a low probability of chance coincidence of the X-ray position with à nIR object in this field. the candidate source is significantly brighter than most other isolated pulsars and brighter than a simple extrapolation of the X-ray spectra to the nIR. making its association with the X-ray source less certain. | While there is a low probability of chance coincidence of the X-ray position with a nIR object in this field, the candidate source is significantly brighter than most other isolated pulsars and brighter than a simple extrapolation of the X-ray spectra to the nIR, making its association with the X-ray source less certain. |
If future observations can confirm the association it seems that an additional emission component will be necessary to explain the excess nIR flux. | If future observations can confirm the association it seems that an additional emission component will be necessary to explain the excess nIR flux. |
The non-detection of the other two sources. aandJ1632—478.. may be understood by the high level of Galactic extinction in their direction and by the intrinsically faint nature of isolated neutron stars. which the compact objects are assumed to be: it may be reasonable to expect the counterparts ofthese sources to be at magnitudes K,z 18.6. | The non-detection of the other two sources, and, may be understood by the high level of Galactic extinction in their direction and by the intrinsically faint nature of isolated neutron stars, which the compact objects are assumed to be; it may be reasonable to expect the counterparts ofthese sources to be at magnitudes $K_s \gtrsim 18.6$ . |
Object hh-540 at redshift 2.80 had in fact already been identified as à good quasar candidate in a variability study. where we compared & magnitudes in frames taken at different epochs throughout the CADIS observing program. | Object h-540 at redshift 2.80 had in fact already been identified as a good quasar candidate in a variability study, where we compared $R$ magnitudes in frames taken at different epochs throughout the CADIS observing program. |
The Seyfert galaxy hh-644 was found by chance among the galaxies we selected for checking our photometric redshift estimates. | The Seyfert galaxy h-644 was found by chance among the galaxies we selected for checking our photometric redshift estimates. |
It has stellar shape and was classified as a starburst galaxy by our algorithm. | It has stellar shape and was classified as a starburst galaxy by our algorithm. |
The quasar 16hh-429 looks morphologically stellar in some filters and extended in others. in the 7? filter and in the A" band. | The quasar h-429 looks morphologically stellar in some filters and extended in others, in the $R$ filter and in the $K^\prime$ band. |
The point source appears to be not precisely centered on the fuzz. | The point source appears to be not precisely centered on the fuzz. |
Our classification assigned a significant likelihood to this object for being a galaxy at 2—1.5. | Our classification assigned a significant likelihood to this object for being a galaxy at $z\approx1.7$. |
We can not decide at this point. whether the visible fuzz around this object is a luminous host galaxy or a foreground object projected onto the line of sight by chance. | We can not decide at this point, whether the visible fuzz around this object is a luminous host galaxy or a foreground object projected onto the line of sight by chance. |
Interesting to note are three pairs of AGNs: Object hh-104 lies outside of the | Interesting to note are three pairs of AGNs: Object h-104 lies outside of the |
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