Datasets:
ReadingTimeMachine
/
rtm-sgt-ocr-v1

Dataset card Data Studio Files Community
1
source
stringlengths
1
2.05k
⌀
target
stringlengths
1
11.7k
This increases the computation time greatly: and since all of the most significant sources were identified with objects whose positions were well known. the smaller bin size was not adopted to give source positions in the 3EG.
This increases the computation time greatly; and since all of the most significant sources were identified with objects whose positions were well known, the smaller bin size was not adopted to give source positions in the 3EG.
See the comment on the source 3EG J0834-4511 (Vela) in the section of particular detections of the 3EG Catalog (Hartman et al.
See the comment on the source 3EG J0834-4511 (Vela) in the section of particular detections of the 3EG Catalog (Hartman et al.
1999).
1999).
Systematies. then. do not pose a major problem for the source location capability of EGRET. even in regions of significant diffuse emission or strong nearby sources (Hartman et al.
Systematics, then, do not pose a major problem for the source location capability of EGRET, even in regions of significant diffuse emission or strong nearby sources (Hartman et al.
1999),
1999).
Most importantly. the error contours for many of the AGNs show that the location capability improves for regions away from the Galactic plane. where most of the blazars are.
Most importantly, the error contours for many of the AGNs show that the location capability improves for regions away from the Galactic plane, where most of the blazars are.
In addition. some of the 3EG-associated AGNs could be false positives (ie. AGNSs that are mis-associated with EGRET sources by a failure of the statistical methods used in. the classification).
In addition, some of the 3EG-associated AGNs could be false positives (i.e. AGNs that are mis-associated with EGRET sources by a failure of the statistical methods used in the classification).
This fact is particularly important for statistical methods based on the relative positions between the candidate and the EGRET source center (see Torres 2003b for a review).
This fact is particularly important for statistical methods based on the relative positions between the candidate and the EGRET source center (see Torres 2003b for a review).
Working with 114 sources above |b]>10°. Punsly (1997) has estimated the number of random coincidences as a function. of the field radius: ~2 (10) quasars with more than | Jy of 5 GHz flux are expected to correlate by random chance if the size of the typical EGRET angular uncertainty is 0.7° (1.7%).
Working with 114 sources above $|b|>10^{{\rm o}}$, Punsly (1997) has estimated the number of random coincidences as a function of the field radius: $\sim 2$ (10) quasars with more than 1 Jy of 5 GHz flux are expected to correlate by random chance if the size of the typical EGRET angular uncertainty is $^{{\rm o}}$ $^{{\rm o}}$ ).
The number of random coincidences increases as the radio-loudness of the AGN decreases (since there are more AGNs with smaller flux).
The number of random coincidences increases as the radio-loudness of the AGN decreases (since there are more AGNs with smaller flux).
This sheds additional doubt on the correlations found beyond the location contours of EGRET sources.
This sheds additional doubt on the correlations found beyond the location contours of EGRET sources.
Available statistics on the arrival directions of the UHECRs reveals no significant correlations above random with BL Lacs nor with any other type of quasars. including EGRET blazar detections.
Available statistics on the arrival directions of the UHECRs reveals no significant correlations above random with BL Lacs nor with any other type of quasars, including EGRET blazar detections.
Furthermore. identifying EGRET sources with BL Lacs just by positional pairing within twice the EGRET error grossly underestimates the goodness of existing gamma-ray data.
Furthermore, identifying EGRET sources with BL Lacs just by positional pairing within twice the EGRET error grossly underestimates the goodness of existing gamma-ray data.
We gratefully acknowledge Elihu Boldt. Francese Ferrer. Haim Goldberg. Tom MeCauley. Andreas Ringwald. Subir Sarkar. Peter Tinyakov. and Alan Watson. for useful discussions/email correspondence.
We gratefully acknowledge Elihu Boldt, Francesc Ferrer, Haim Goldberg, Tom McCauley, Andreas Ringwald, Subir Sarkar, Peter Tinyakov, and Alan Watson, for useful discussions/email correspondence.
We further acknowledge Alan Watson for his kind permission to use the Haverah Park data.
We further acknowledge Alan Watson for his kind permission to use the Haverah Park data.
The work of D.E.T. was performed under the auspices of the U.S. D.O.E. (NNSA). by University of California Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48.
The work of D.F.T. was performed under the auspices of the U.S. D.O.E. (NNSA), by University of California Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48.
The research of S.R. and L.A.A was partially supported by the US National Science Foundation (NSF) under grant No.
The research of S.R. and L.A.A was partially supported by the US National Science Foundation (NSF) under grant No.
PHY-0140407.
PHY-0140407.
density at NS.d4-Cllz is 3.4 mw and so 2 mv of Hlux has been resolved out: similarly. assuming a spectral index of -l suggests that ~5 my has been resolved out.
density at 8.4-GHz is $\sim 3-4$ mJy and so $\sim2$ mJy of flux has been resolved out; similarly, assuming a spectral index of -1 suggests that $\sim5$ mJy has been resolved out.
These estimates require that no flux is resolved out at 4.9-CillIz. a reasonable assumption given the uniformity of the southern middle lobe in the 64,4egsspocg; Map.
These estimates require that no flux is resolved out at 4.9-GHz, a reasonable assumption given the uniformity of the southern middle lobe in the $\alpha_{1.4-GHz/4.9-GHz}$ map.
While the bright core suggests the possibility that the inner lobes are still receiving energy. via jets (as also found in other objects. c.g. JOOLL|3224: Saikia ct al.
While the bright core suggests the possibility that the inner lobes are still receiving energy via jets (as also found in other objects, e.g. J0041+3224; Saikia et al.
2006). the absence of hotspots in the outer ancl possibly the middle lobes suggests that these structures are no longer supplied with energv.
2006), the absence of hotspots in the outer and possibly the middle lobes suggests that these structures are no longer supplied with energy.
Such à statement is supported. by the steep spectral indices presented in Fie.
Such a statement is supported by the steep spectral indices presented in Fig.
2. (middle lobes) and the table of observed. parameters (Table 2)). which includes
\ref{alpha} (middle lobes) and the table of observed parameters (Table \ref{data}) ), which includes
The stellar content and. hence the spectral energy. cistribution (SED) of a galaxy. clepeuds on παν factors.
The stellar content and hence the spectral energy distribution (SED) of a galaxy depends on many factors.
Accurate predictions of galaxy SEDs require sound theories of stellar evolution
Accurate predictions of galaxy SEDs require sound theories of stellar evolution
the reservoir until it is depleted at which point any further gas accreted is assumed primordial.
the reservoir until it is depleted at which point any further gas accreted is assumed primordial.
Recently. ?. have studied the ellects of recycling on the SETts and stellar mass function of galaxies in cosmological hydrodynamical simulations ancl have found that it is the dominant factor in galaxy growth at 2x]. ejecta being the important factor at 2>2.
Recently, \citet{opp} have studied the effects of recycling on the SFRs and stellar mass function of galaxies in cosmological hydrodynamical simulations and have found that it is the dominant factor in galaxy growth at $z\le1$, ejecta being the important factor at $z\ge2$.
Hence. in this work we focus on the supernova feedback ellicieney. ane do not vary €. holding it constant at the fiducial value. 20.3. so that during any gas re-accretion process. is drawn from the reservoir (provided it is not depleted). the remainder being of primordial metallicity.
Hence, in this work we focus on the supernova feedback efficiency and do not vary $\zeta$, holding it constant at the fiducial value, $0.3$, so that during any gas re-accretion process, is drawn from the reservoir (provided it is not depleted), the remainder being of primordial metallicity.
The gas metallicity must be determined using strong line metallicity clagnostics (2). which relics on the fact that the ratio of various strong optical emission lines depend: upon the eas metallicity in a known manner.
The gas metallicity must be determined using strong line metallicity diagnostics \citep{amaze} which relies on the fact that the ratio of various strong optical emission lines depend upon the gas metallicity in a known manner.
Thus these ratios must be calibrated. against metallicitv.
Thus these ratios must be calibrated against metallicity.
. Calibrations have only been performed in. narrow metallicity ranges.
Calibrations have only been performed in narrow metallicity ranges.
These calibrations are often inconsistent with cach other ancl can lead to cilferent metallicity olfsets of up to 0.7 dex and the dilference in the shape of the curve is often large (?)..
These calibrations are often inconsistent with each other and can lead to different metallicity offsets of up to $0.7$ dex and the difference in the shape of the curve is often large \citep{kew08}.
Since data measured at different redshifts may be measured using cilfercnt optical lines it is essential to ensure a correct intercalibration between the data fits so that the correct evolution of the relation can be seen.
Since data measured at different redshifts may be measured using different optical lines it is essential to ensure a correct intercalibration between the data fits so that the correct evolution of the relation can be seen.
These intercalibration issues are tackled by 7. and by 2.. who take a Large sample of local galaxies spanning a wide range of metallicitics (7.2«12|log(O/H)9.2. accurately measured by using both the electron temperature method and. photoinoization models) and cross-calibrate the various strong line ratio diagnostics on the same metallicity We take as our observed trend. the AAMIAZE (7). mass-metallicity relation wwhere logAdy and Au are free parameters that must. be determined at each redshift to obtain the best-fitting to the observed. data and. are shown in Table 1..
These intercalibration issues are tackled by \citet{Nagao} and by \citet{amaze}, who take a large sample of local galaxies spanning a wide range of metallicities $7.2< 12+\log(O/H)<9.2$, accurately measured by using both the electron temperature method and photoinoization models) and cross-calibrate the various strong line ratio diagnostics on the same metallicity We take as our observed trend the AMAZE \citep{amaze} mass-metallicity relation where $\log M_\mathrm{0}$ and $K_\mathrm{0}$ are free parameters that must be determined at each redshift to obtain the best-fitting to the observed data and are shown in Table \ref{tab:cal}.
The calibration constants at z0.07 were derived using the data from ?.. the constants at z227 were found using the data from ? and the constants corresponding to z=3.54 were calculated using cata from ?..
The calibration constants at $z=0.07$ were derived using the data from \citet{kew08}, the constants at $z=2.27$ were found using the data from \citet{erb06} and the constants corresponding to $z=3.54$ were calculated using data from \citet{amaze}.
In this section we test the cllects of changing the parameters. in order to identify those that may improve the agreement with observations.
In this section we test the effects of changing the parameters, in order to identify those that may improve the agreement with observations.
A more quantitative discussion. will involve only these parameters.
A more quantitative discussion will involve only these parameters.
Initially all qualitative results were obtained using the Salpeter EME (equation 1)) however the elfect of changing to the Ixenicutt IME (equation 2)) is investigated in section 4.2..
Initially all qualitative results were obtained using the Salpeter IMF (equation \ref{eq:salp}) ) however the effect of changing to the Kenicutt IMF (equation \ref{eq:ken}) ) is investigated in section \ref{sec:kenimf}.
Holding 3. ο at their fiducial values (2).. the parameter à was varied over the range 0.01<a«0.05 (ο investigate he effects of changing the star formation cllicicney on the sreclicted mass metallicity relation.
Holding $\beta$, $\epsilon$ at their fiducial values \citep{galics1}, the parameter $\alpha$ was varied over the range $0.01<\alpha<0.05$ to investigate the effects of changing the star formation efficiency on the predicted mass metallicity relation.
Fig.
Fig.
1: shows the output or galaxies at. redshift 27 plotted as 12|log(O/1) Vs.
\ref{fig:alpha1} shows the output for galaxies at redshift $2.27$ plotted as $12+\log\left(O/H\right)$ Vs.
ogCAL,AL.) where M, is the stellar mass.
$\log\!\left( M_\star/M_\odot\right)$ where $M_\star$ is the stellar mass.
Also plotted are he observations at 2227 from? as well as the calibrated »st-fitting trend. (equation 5)) at redshift 2.27-.-d and 0.07.
Also plotted are the observations at $z=2.27$ from \citet{erb06} as well as the calibrated best-fitting trend (equation \ref{eq:cal}) ) at redshift $2.27$ and $0.07$.
The corresponding plot for galaxies at redshift, 3.54 is shown in Lig. 2..
The corresponding plot for galaxies at redshift $3.54$ is shown in Fig. \ref{fig:alpha2}.
We note that. although the minimunr xwvonie mass is 2x10AZ... it is possible to have galaxies whose stellar mass is less than this in the sample provided hat their barvonic mass exceeds this minimum value.
We note that, although the minimum baryonic mass is $2\textrm{x}10^{9}M_\odot$, it is possible to have galaxies whose stellar mass is less than this in the sample provided that their baryonic mass exceeds this minimum value.
The Mots show that increasing à has the ellect of spawning a similar number of galaxies (at the same redshift) that lve on average a higher mass ancl metallicity.
The plots show that increasing $\alpha$ has the effect of spawning a similar number of galaxies (at the same redshift) that have on average a higher mass and metallicity.
Increasing o increases the SER. in direct. proportion thus in the same Llubble time we have more stars formed and a larger »woportion at a later stage in. their ife and. so the stellar mass and metallicity is increased.
Increasing $\alpha$ increases the SFR in direct proportion thus in the same Hubble time we have more stars formed and a larger proportion at a later stage in their life and so the stellar mass and metallicity is increased.
We note from Fig.
We note from Fig.
2 that he observed: mass-metallicity relation (?) would. be best itted using a low star formation ellicicney for low-mass ealaxies and a high star formation ellicicney for. high-mass galaxies.
\ref{fig:alpha2} that the observed mass-metallicity relation \citep{amaze} would be best fitted using a low star formation efficiency for low-mass galaxies and a high star formation efficiency for high-mass galaxies.
This supports the findings of ? who argue that ow-nmass galaxies are characterized ow low star formation elliciencies inhibiting chemical evolution.
This supports the findings of \citet{amaze} who argue that low-mass galaxies are characterized by low star formation efficiencies inhibiting chemical evolution.
We will return to his issue later in section ??..
We will return to this issue later in section \ref{sec:discussion}.
From a formal point of view. if we quantify the agreement between model predictions and. data in terms of the X7 we have values that monotonically decrease with increasing o. simply because the normalization of the predicted niass-metallicity relation increases and. on average. more model ealaxies are in better agreement with the data.
From a formal point of view, if we quantify the agreement between model predictions and data in terms of the $\chi^2$, we have values that monotonically decrease with increasing $\alpha$, simply because the normalization of the predicted mass-metallicity relation increases and, on average, more model galaxies are in better agreement with the data.
This trend. however. has the elect of predicting too many small ealaxies al ~3 that exhibit the metallicity of à tvpical z~2 galaxy of the same mass.
This trend, however, has the effect of predicting too many small galaxies at $z\sim3$ that exhibit the metallicity of a typical $z\sim2$ galaxy of the same mass.
This trend. is already present at a0.06 without inducing any improvement of the slope of the predicted. relation.
This trend is already present at $\alpha=0.06$ without inducing any improvement of the slope of the predicted relation.
When discussing the vields. we showed that we adopt quite a conservative value for the O xoduction. therefore we believe hat values for à0.05 should be avoided even if they [ead to a low value X7.
When discussing the yields, we showed that we adopt quite a conservative value for the O production, therefore we believe that values for $\alpha>0.05$ should be avoided even if they lead to a low value $\chi^2$.
Also. he reader should note here that during the preparation of the manuscript. several papers have introduced. a more robust way to explore the parameter space and statistically iuidle the comparison between model. predictions. and observations (see.forexample.??)..
Also, the reader should note here that during the preparation of the manuscript, several papers have introduced a more robust way to explore the parameter space and statistically handle the comparison between model predictions and observations \citep[see, for example,][]{bower,lu}.
In particular. ? argue hat the procedure adopted here (namely varving only one xwanmeter at a time) does not allow one to uniformly explore he parameter space and that the 7best-fitting by eve” values do not always coincide with the point that has the maximum ikelihood in the parameters multidimensional phase space.
In particular, \citet{lu} argue that the procedure adopted here (namely varying only one parameter at a time) does not allow one to uniformly explore the parameter space and that the “best-fitting by eye” values do not always coincide with the point that has the maximum likelihood in the parameters multi-dimensional phase space.
On the other hand. the procedure ?/— advocate may [ead
On the other hand, the procedure \citet{lu} advocate may lead
orbit).
orbit).
The methods based on observations of molecular gas and dust would refer to the deser material. probably lying close to the orbital plane. whereas the radio continuum data would probe the low-mass regions.
The methods based on observations of molecular gas and dust would refer to the denser material, probably lying close to the orbital plane, whereas the radio continuum data would probe the low-mass regions.
As a result. one should get higher mass values from molecular lines and dust than from radio continuum data.
As a result, one should get higher mass values from molecular lines and dust than from radio continuum data.
Our rates from CO are about 2 orders of magnitude higher than published values based on radio data. in agreement with these expectations.
Our rates from CO are about 2 orders of magnitude higher than published values based on radio data, in agreement with these expectations.
The poor pprofiles observed in CH Cyg prevent any detailed fitting of the line shape.
The poor profiles observed in CH Cyg prevent any detailed fitting of the line shape.
Both lines show roughly a central peak and could be compatible with the emission of a region with significant velocity gradient.
Both lines show roughly a central peak and could be compatible with the emission of a region with significant velocity gradient.
We can derive some characteristics of the emitting region from the line intensity.
We can derive some characteristics of the emitting region from the line intensity.
First of all. we can see that the lintensity ratio is relatively high. compatible with the optically thick ratio. ~ 3.5 33.1; see also discussion for R Agr in 4.1).
First of all, we can see that the intensity ratio is relatively high, compatible with the optically thick ratio, $\sim$ 3.5 3.1; see also discussion for R Aqr in 4.1).
We also note that the component separation in. the object is ~ 9 AU. smaller than that of R Aqr.
We also note that the component separation in the object is $\sim$ 9 AU, smaller than that of R Aqr.
Therefore we can assume that both lines are optically thick and come from a very compact region.
Therefore we can assume that both lines are optically thick and come from a very compact region.
From our discussion in 33.1. we can deduce that the observed line intensities are compatible with an emitting region size (typical diameter) of about 10 AU (typical radius ~ 5 AU. somewhat smaller than the component separation). and typical kinetic temperature of about KK. Note that the detected profiles are. within the uncertainties, quite wide. suggesting that high expansion velocities are present in the CO-rich shells. ~ 25. even larger than those measurec for R Aqr.l
From our discussion in 3.1, we can deduce that the observed line intensities are compatible with an emitting region size (typical diameter) of about 10 AU (typical radius $\sim$ 5 AU, somewhat smaller than the component separation), and typical kinetic temperature of about K. Note that the detected profiles are, within the uncertainties, quite wide, suggesting that high expansion velocities are present in the CO-rich shells, $\sim$ 25, even larger than those measured for R Aqr.;
ifetime): we deduce. following the prescriptions in 33.1. 22 107!..
we deduce, following the prescriptions in 3.1, 2 $^{-5}$.
We suggest that the high values of the mass-loss rate and expansion velocity are partially due to the fact that the CH Cyg system is tighter than that of R Aqr.
We suggest that the high values of the mass-loss rate and expansion velocity are partially due to the fact that the CH Cyg system is tighter than that of R Aqr.
The values derived here for the mass-loss rate and typical temperature in the inner shells are quite similar to those found by Taranova Shenavrin (2007) from analysis of the dust FIR emission of recently ejected material.
The values derived here for the mass-loss rate and typical temperature in the inner shells are quite similar to those found by Taranova Shenavrin (2007) from analysis of the dust FIR emission of recently ejected material.
Our mass-loss rates are also compatible with the total dust mass derived by Kenyon et ((1988) and Hinkle et ((2009). if we assume that dust emission comes from inner shells not much larger than those we are detecting in CO emission.
Our mass-loss rates are also compatible with the total dust mass derived by Kenyon et (1988) and Hinkle et (2009), if we assume that dust emission comes from inner shells not much larger than those we are detecting in CO emission.
The other molecular observations in R Aqr. CH Cyg and HM Sge did not yield detections.
The other molecular observations in R Aqr, CH Cyg and HM Sge did not yield detections.
The upper limits obtained for lines are compatible with aabundance ratios larger than. 10. as usually found in similar objects.
The upper limits obtained for lines are compatible with abundance ratios larger than 10, as usually found in similar objects.
The nondetection of tto a limit of Τρί2-1) < 0.02 K in HM Sge. a source
The nondetection of to a limit of $T_{\rm mb}(\jdu)$ $<$ 0.02 K in HM Sge, a source
clusty disk.
dusty disk.
In total. at least half of the active earlv-tvpe galaxies exhibit some evidence [ου dust. disks and of these have tightly wound spirals in regular disks.
In total, at least half of the active early-type galaxies exhibit some evidence for dust disks and of these have tightly wound spirals in regular disks.
These later dust structures are interesting because tightly wound dust structures are generally observed in the most aNXisvinimetric (1.e.. unbarred) Iate-tvpe galaxies aud suggest (he presence of long-lived structures (Peeples&Martini2006).
These later dust structures are interesting because tightly wound dust structures are generally observed in the most axisymmetric (i.e., unbarred) late-type galaxies and suggest the presence of long-lived structures \citep{peeples06}.
. The presence of any dust structures in each galaxy is indicated in column 11 of Tables 1. and 2.. where we report the projected radial extent of each dust feature in kiloparsecs.
The presence of any dust structures in each galaxy is indicated in column 11 of Tables \ref{tab-active} and \ref{tab-control}, where we report the projected radial extent of each dust feature in kiloparsecs.
This radius was estimated by visual inspection of the dieital images.
This radius was estimated by visual inspection of the digital images.
A x sign means that the radius of the structure is not clear. and may extend bevond the borders of the image.
A $\times$ sign means that the radius of the structure is not clear, and may extend beyond the borders of the image.
For the late-tvpe galaxies we have not measured the radius ol the dust structure as in most cases it does extend bevond the borders of the images.
For the late-type galaxies we have not measured the radius of the dust structure as in most cases it does extend beyond the borders of the images.
The dust disks aud spirals have a mean size of 0.43840.37 kkpe ancl 0.6940.63 kkpe respectively for the early-type active galaxies.
The dust disks and spirals have a mean size of $\pm$ kpc and $\pm$ kpc respectively for the early-type active galaxies.
These structures therefore appear to be confined to the circumnuclear region or central kiloparsec. alühough these observations are less sensitive {ο dust on larger scales due to a decrease in signal-to-noise ratio.
These structures therefore appear to be confined to the circumnuclear region or central kiloparsec, although these observations are less sensitive to dust on larger scales due to a decrease in signal-to-noise ratio.
The position angles of the clusty disks in the eurl-tvpes. if apparent. are generally. aligned. with (he position angle of the large-scale isophotes.
The position angles of the dusty disks in the early-types, if apparent, are generally aligned with the position angle of the large-scale isophotes.
Some exceptions include orthogonal dust disks in NGC 2787. NGC 4111. and NGC 4143.
Some exceptions include orthogonal dust disks in NGC 2787, NGC 4111, and NGC 4143.
In addition to circumnuclear dust. our structure maps also reveal (he presence of nuclear stellar disks in many galaxies.
In addition to circumnuclear dust, our structure maps also reveal the presence of nuclear stellar disks in many galaxies.
We have found disks in at least 13 οἱ the 34 )) earlv-tvpe inactive galaxies. while we found nuclear stellar disks in only one of the 34 (3%)) early-type aclive galaxies.
We have found disks in at least 13 of the 34 ) early-type inactive galaxies, while we found nuclear stellar disks in only one of the 34 ) early-type active galaxies.
Many. of these nuclear stellar disks were identilied in previous work. such as 44570. 44621 and 55308 by Ixrajnovié&Jaffe(2004).. which emploved elliptical isophote fits to identifv these disks.
Many of these nuclear stellar disks were identified in previous work, such as 4570, 4621 and 5308 by \citet{krajnovic04}, which employed elliptical isophote fits to identify these disks.
As we have identified a similar fraction of stellar disks. structure maps may be as sensitive to nuclear disks as isophote fitting.
As we have identified a similar fraction of stellar disks, structure maps may be as sensitive to nuclear disks as isophote fitting.
This is somewhat surprising. as structure maps are best suited to the detection of features on the scale of the point spread function.
This is somewhat surprising, as structure maps are best suited to the detection of features on the scale of the point spread function.
The appearance of the stellar disks in (he structure maps may (herefore indicate that (μον are nearly edge on. as is the case for elliptical isophote fits.
The appearance of the stellar disks in the structure maps may therefore indicate that they are nearly edge on, as is the case for elliptical isophote fits.
Consistent with this interpretation. nearly all of the nuclear stellar clisks in our sample have verv large axis ratios.
Consistent with this interpretation, nearly all of the nuclear stellar disks in our sample have very large axis ratios.
The detectability of stellar disks in early-twpe galaxies was mocdeled in detail bv Rix&White(1990).. who found that the observed. fraction is consistent with the presence of a nuclear stellar disk in every eurlv-tvpe galaxy.
The detectability of stellar disks in early-type galaxies was modeled in detail by \citet{rix90}, who found that the observed fraction is consistent with the presence of a nuclear stellar disk in every early-type galaxy.
The apparent nuclear stellar disks in these galaxies could also be nuclear stellar bars (e.g..Erwin&Sparke2002).
The apparent nuclear stellar disks in these galaxies could also be nuclear stellar bars \citep[e.g.,][]{erwin02}.
. To determine if (his is the case we measured (he position angle of each of (he nuclear stellar disks and compared it with the position angle of the ealaxv isophotes on large scales.
To determine if this is the case we measured the position angle of each of the nuclear stellar disks and compared it with the position angle of the galaxy isophotes on large scales.
In all cases the nuclear stellar disk was aligned. with the position angle on larger scales. which suggests that (μον are not nuclear bars.
In all cases the nuclear stellar disk was aligned with the position angle on larger scales, which suggests that they are not nuclear bars.
Surprisinely. (he position angles of the nuclear stellar disks in five out of five elliptical galaxies also agree
Surprisingly, the position angles of the nuclear stellar disks in five out of five elliptical galaxies also agree