The reddest ISO–2MASS quasar Based on observations made with ESO Telescopes at La Silla and Paranal under programme IDs 275.A-5064 and 075.A-0374, with the Spitzer Space Telescope, which is operated by the JPL, CALTECH under a contract with NASA, and obtained at CTIO a division of NOAO, which is operated by AURA under cooperative agreement with the National Science Foundation.

The reddest ISO–2MASS quasar 1

Key Words.:
Galaxies: active – quasars: general – Infrared: galaxies

Abstract

Context:While there is growing consensus on the existence of numerous dust–enshrouded red quasars, their discovery and detailed exploration is still an observational challenge. In the course of the near–mid–infrared AGN search combining the 6.7 m ISOCAM Parallel Survey and 2MASS we have discovered 24 type –1 quasars about a third of which are too red to be discriminated by optical/UV search techniques.

Aims:Here we report on a detailed case study of the reddest type –1 quasar of our sample, 2MASS J234106670914327 (for short J2341) at redshift with M and . This source has a very red optical appearance but lacks the far-infrared emission typically seen in known dust enshrouded AGN. Therefore we here explore its enigmatic nature.

Methods:We performed spectroscopy in the optical with VLT/FORS1 and in the mid–infrared (m) with the Spitzer Space Telescope as well as near–infrared (NIR) imaging with ISPI at the CTIO 4m–telescope. To explain the red optical continuum of the quasar we examine nuclear dust reddening of an intrinsically blue quasar continuum in combination with dilution by stellar light of the host galaxy.

Results:The optical and NIR observations reveal a star forming emission–line galaxy at the same redshift as the quasar with a projected linear separation of 18 (6.7 kpc). The quasar and its companion are embedded in diffuse extended continuum emission. Compared with its companion the quasar exhibits redder optical–NIR colours, which we attribute to hot nuclear dust. The mid–infrared spectrum shows only few emission lines superimposed on a power–law spectral energy distribution typically seen in type –1 AGN. However, the lack of strong far–infrared emission suggests that our potentially interacting object contains much less gas and dust and is in a stage different from dust reddened ULIRG–AGN like Mrk 231. The optical spectrum shows signatures for reddening in the emission–lines and no post–starburst stellar population is detected in the host galaxy of the quasar. The optical continuum emission of the active nucleus appears absorbed and diluted.

Conclusions: Even the combination of absorption and host dilution is not able to match J2341 with standard quasar templates. While the BLR shows only a rather moderate absorption of E, the continuum shorter than requires strong obscuration with E, clearly exceeding the constraints from the low upper limit on the silicate 9.7 m absorption. This leads us to conclude that the continuum of the quasar J2341 is intrinsically redder than that of typical quasars.

1 Introduction

Pure optical quasar surveys find QSOs with essentially blue continua (e.g. Schmidt & Green (1983); Wolf (2005)). However, investigations including the radio, X–ray and infrared have revealed a substantial fraction of dust–reddened AGN missed by optical surveys (Low et al. (1988); Gregg et al. (2002); Maiolino et al. (2003); Glikman et al. (2004); Lacy et al. (2004)). We have combined the ISOCAM Parallel Survey at 6.7 m (Siebenmorgen et al. (1996)) with the 2MASS survey (Skrutskie et al. (2006)) in order to obtain a powerful tool to search for AGN by means of their infrared colours ( and ; Haas et al. (2004)). In fact, in a high galactic latitude area of  10 deg we found % more type –1 quasars per square degree down to  18 mag than e.g. the SDSS DR3 quasar survey (Leipski et al. (2005)). The quasars found by our NIR/MIR method show a variety of spectral shapes, in particular in the optical. Some of the ISO–2MASS objects are too red to be recognised as quasars by current optical strategies, probably because of dust extinction. Since the NIR and MIR colours of quasars are different from those of stars, infrared selection enables the detection of optically red quasars (Cutri et al. (2002); Smith et al. (2003); Leipski et al. (2005); Lacy et al. (2007)).

From our sample of 77 AGN candidates 24 turned out to be type –1 AGN. They span a range of optical colours from blue quasar–typical ones to very red ones similar to those found in dust–enshrouded ULIRG-AGN. The reddest quasar of our sample is 2MASS J234106670914327 (hereafter called J2341) at a moderate redshift . Thus, its red photometric appearance is not due to high redshift.

Alternatively to the classical M mag quasar definition, its absolute –band brightness of M =  mag qualifies J2341 as a QSO. The absolute SDSS i magnitude of M mag  and an [O iii] 5007 luminosity of  erg s places J2341 at the low luminosity end of the total luminosity distribution of quasars found in the SDSS, but at intermediate values for objects in the regime (Schneider et al. (2007)). While no radio counterpart is listed by NVSS (translating to  mJy; Condon et al. al. (1998)), ROSAT HRI observations give a soft X–ray luminosity of  erg s, similar to that of low redshift PG–quasars. The galactic foreground extinction is E (Schlegel et al. (1998)).

The low IRAS 60 m upper limit  mJy suggests that J2341 is different from known ULIRG-AGN. If this is true, then its red optical colours are puzzling. Therefore we performed a detailed case study of J2341, using optical VLT spectra, near–infrared imaging from the CTIO 4m telescope and mid–infrared spectra from the Spitzer Space Telescope.

2 Observations

The quasar nature of J2341 was discovered on spectra taken with EMMI at the ESO/NTT telescope during the optical follow–up spectroscopy of our MIR selected AGN candidates. We used a 15 wide long slit oriented along the parallactic angle (slit–loss effects due to atmospheric dispersion are minimised by such a slit orientation) and centred on the peak of the apparent brightness distribution (Fig. 1). These observations were obtained before the object was recognised as a double source. The slit width in combination with Grism#2 results in a spectral resolution of km s. The integration time was min.

Figure 1: Contour plot of the J2341 “system” from the 30 sec VLT –band acquisition image. The contour levels have been chosen to highlight the extended emission. The image shows 18″  18″ (90 px  90 px). The positions and widths of the VLT slit (p.a. 120°; 13 width) and the NTT slit (p.a. 155°; 15 width) are indicated by the lightly shaded rectangles. The darker shaded areas indicate the positions and widths of the extraction regions for the spectra used in this paper.

In order to check morphological details and the NIR photometry, we have obtained images with ISPI at the CTIO 4m–Blanco telescope. These observations were performed under stable seeing conditions (FWHM 1) with a total on–source integration time of 15 min in each filter. The images were reduced using standard IRAF procedures.

After detecting that J2341 may be a double source, we have further obtained optical spectra with VLT/FORS1 in order to explore the nature of J2341 and its putative companion. The 13 wide slit was oriented to cover both objects (Fig. 1) and an atmospheric dispersion corrector was used for the min observation. In combination with grism GRIS_300V the observations yield a spectral resolution of km s.

The optical spectra were reduced using standard procedures within the ESO/MIDAS package. Since no spatial structure could be identified on the 2D spectroscopic frames from the NTT run we combined all the flux into a single spectrum. This procedure may include contributions from the underlying host galaxy and from the companion, diluting the QSO signatures in the final NTT spectrum. The spectroscopic observations with the VLT were able to spatially resolve both objects since the slit was optimally oriented. We searched for the brightest spectral column in broad line flux and in continuum for the QSO and the companion, respectively. We extracted 3–pixel wide columns (0.2″/px) into single spectra, each corresponding to only 06 spatially. Since the seeing was  10 during the observations this choice reduces the flux in the extracted spectra but minimises the contributions from the adjacent source while providing adequate S/N ratios.

We also obtained a low–resolution m MIR spectrum of J2341 using IRS (Houck et al. (2004)) aboard Spitzer Space Telescope (Werner et al. (2004)) with total integration times of 240 sec and 480 sec for SL and LL, respectively. We used data processed by version S15.3.0 of the IRS pipeline and performed calibration and extraction of the spectra within SPICE.

3 Comparison of the NTT and VLT spectra

Here we briefly consider whether observational effects or host galaxy contamination is important for the red appearance of the quasar spectrum and how far the quasar and companion spectra may be contaminated by each other.

In Fig. 2 we plot the NTT spectrum (extracted through a large aperture) over the VLT spectrum of the QSO (extracted through a narrow aperture). The shape of the continuum agrees very well for both observations. We conclude that the red continuum is intrinsic to the source and not an artifact from the data reduction or due to slit–loss effects. In addition, the red optical continuum is also evident from USNO and SDSS photometry (e.g. Fig. 3 in Leipski et al. (2005)).

Figure 2: Comparison of the VLT spectrum (dotted line) and the NTT spectrum (solid line; scaled to match the continuum between 4000 and 6000 ).

Compared with the VLT spectrum, the NTT spectrum includes more flux from the underlying host galaxy and potentially some flux from the companion as well. Therefore it shows more pronounced and even additional stellar absorption lines. The increased continuum flux also results in smaller equivalent widths (EWs) of the emission lines (Fig. 2).

Despite the stronger stellar contribution in the NTT spectrum, the shape of the continuum is the same for both the VLT and NTT spectra. This suggests that the influence of stellar light contributions on the shape of the observed continuum can be significant even for the nuclear VLT spectrum. We will address the underlying host galaxy further in Section 4.4.2.

In Figs. 3 and 4 we show the VLT spectra of the QSO and its companion. These spectra were extracted through narrow apertures to minimise contaminations from each other. The absence of broad emission–line components and emission from the highly ionised inner parts of the narrow–line region (e.g. [Ne v]) in the spectrum of the companion strongly argues against significant contributions from emission of the QSO. The QSO spectrum does not show signs for higher order Balmer absorption lines which are on the other hand prominent in the companion. This supports our conclusion that the spectra of the QSO and the companion show the intrinsic features of the respective source and that they are not significantly contaminated by each other.

4 Results and Discussion

The inspection of the frames and the –band acquisition image (30 sec integration time) reveals a nearby faint object approximately 18 north–west of J2341 (Figs. 1 and 3; position angle  294 deg), which could be a physically interacting companion galaxy. The VLT spectra reveal that both objects lie at the same redshift ( 0.236). This and the small projected separation of 18 ( 6.7 kpc) suggests that they are in fact interacting. This is further supported by recent and ongoing star formation in the companion (Sect. 4.2). The images do not show clear morphological peculiarities or tidal tails but both galaxies are embedded in weak extended emission which is best seen in the –band image (Fig. 1). In order to assess the amount of extended emission we subtracted two gaussian point sources, one for the QSO and one for the companion. The gaussian width was determined from nearby stars and fits their profiles as well as that of the QSO flux peak. Table 1 lists the resulting photometry for the entire system as well as the flux ratios QSO/companion and nuclear/total. Our analysis shows that the contribution of the extended emission is largest in and .

In the following discussion, the name “J2341” will refer to the quasar and the secondary object is called “companion”.

4.1 The quasar

The spectrum of J2341 shows broad Balmer emission lines (FWHM km/s, rest frame) and a red optical continuum (Fig. 2). This is unusual for a type–1 AGN. We just note that some unusual broad absorption line QSOs (BALQSOs) show very red SEDs due to wide, overlapping BAL troughs in the ultraviolet (e.g. Hall et al. (2002); Meusinger et al. (2005)). While the continuum of J2341 is smooth and does not exhibit any indications for BAL structures over the wavelength range covered by our spectra, the presence of BALs at  Å cannot be excluded. It is well known that BALQSOs tend to be more dust reddened than non–BALQSOs (Reichard et al. (2003)).

Figure 3: –band surface plot and spectra of the two objects obtained with FORS1/VLT. The flux is given in 10 erg sec cm Å.

Figure 5 displays the mean SDSS quasar template (Vanden Berk et al. (2001)) over the spectrum of J2341. While J2341 agrees with the optical quasar template at , it is redder shortwards of that wavelength where the continuum of classical quasars is dominated by blue, power–law like emission. J2341 is also redder than reddened quasars usually found using optical multi–colour selection techniques (e.g. Richards et al. (2003)). The flux ratio of the broad Balmer emission lines is larger for J2341 than for the template, indicating that the BLR of J2341 is also reddened. We will address the reddening further in Section 4.4.1.

Figure 4 shows an enlarged view of the blue portion of the quasar spectrum. Broad Balmer emission lines and Fe ii emission are detected, as well as low and high ionisation forbidden lines from the narrow–line region (e.g. [Ne v], [O ii], [Ne iii], [O iii]). We also detect Ca II K as an absorption feature from the host galaxy. The presence of Ca II K and the absence of higher order Balmer absorption suggests that J2341 does not have a strong contribution from a young–to–intermediate age stellar population (Gyr).

In the mid infrared (Fig. 6) J2341 shows a power–law continuum typical for classical AGN (e.g. Weedman et al. (2005); Ogle et al. (2006); Buchanan et al. (2006)). We see the [O iv] emission line at the 5- level. The high ionisation [Ne v] lines are not detected in the MIR, although prominent in the optical spectrum (Fig. 4). We also do not detect the low ionisation emission lines [Ne ii] and [Ne iii]. The detection of [O iv] and the upper limits on the [Ne v] lines are consistent with the fact that in AGN [O iv] is usually the brightest MIR line, on average about three times brighter than the [Ne v] lines (e.g. Haas et al. (2005)). On the other hand, weak PAH emission features at 7.7 m and 11.3 m are seen. Albeit of marginal significance, they are present at both nod positions of the spectral frames.

Figure 4: Blue portion of the spectra of the quasar and its companion.

The slits of IRS (36 and 106 for SL and LL, respectively) include the quasar as well as its companion, but the MIR continuum is likely to be dominated by dust emission from the quasar itself, which is already 5.5 times brighter at than the companion (Tab. 1).

With  erg/s the MIR luminosity of J2341 is relatively low compared to powerful AGN but the source can still be considered MIR strong (Ogle et al. (2006)). J2341 turns out to be almost a factor of 10 less luminous in the MIR than type –2 AGN at similar redshift which were found in the ISO–2MASS survey (Leipski et al. (2007)).

It is expected that the interaction of both objects triggers enhanced nuclear star formation, when gas and dust are concentrated in the central regions. To study the rate of star formation in quasars, Ho ((2005)) examined the [O ii]/[O iii] flux ratio of PG quasars. Low ratios between 10% and 30% are consistent with AGN origin. Using this method for J2341 the low [O ii]/[O iii] ratio of 10% does not indicate strong ongoing star formation.

In Fig. 6 we overplot the IRS spectrum of the broad–line AGN/ULIRG Mrk 231 (Weedman et al. (2005)). In contrast to J2341, Mrk 231 shows silicate absorption, although broad permitted lines are present in its optical spectrum. In J2341 on the other hand it seems that there is not enough dust between the putative torus (as the source of the MIR continuum emission) and the observer to produce significant silicate absorption. Mrk 231 also exhibits a significant FIR excess that indicates powerful hidden starbursts. J2341 has relatively low FIR emission as derived from IRAS–ADDSCANs ( mJy) and from the flat m slope of the MIR spectrum (Fig. 6). Therefore, dusty starbursts as found in Mrk 231 are not present, as already inferred from the optical spectrum. We suggest that in J2341 the total amount of dust and gas for fuelling starbursts, which can be triggered by the interaction, is low.

Figure 5: Spectra of J2341 and the mean SDSS quasar template of Vanden Berk et al. ((2001)). The SDSS spectrum was scaled to match J2341 in H.

4.2 The companion

The spectrum of the companion is reminiscent of an e(c) galaxy with rather strong H absorption (Dressler et al. (1999)). As a result of a starburst in the past a significant population of A type stars exist in the companion as traced by prominent Balmer absorption lines (Fig. 4). We can speculate that the first encounter of this galaxy with the quasar has initiated a burst of star formation in the companion resulting in the strong population of A stars observed today.

Ongoing star formation is traced by emission lines like [O ii] and H. This star formation is likely to be triggered by the interaction. The observed H emission could in principle be a contamination from an extended narrow–line region of the quasar. However, the low observed [O iii] flux and the very different [O ii]/[O iii] flux ratio suggests that most of the line emission is intrinsic to the companion. While the H/H ratio appears to be large suggesting significant reddening, the H line in this object is affected by strong stellar Balmer absorption masking the intrinsic reddening.

The absence of strong FIR emission as evident from the Spitzer spectrum at m (Fig. 6) suggests that there is no strong, dust–enshrouded starburst in the companion, which could contribute to the FIR flux. Since ongoing star formation is weak in the host galaxy of the quasar but clearly observed in the companion, most of the PAH features detected in the MIR spectrum could actually arise in the companion.

Figure 6: IRS/Spitzer spectra of J2341 and Mrk 231 scaled to match J2341 at 15 m. The positions of important emission lines are marked.

4.3 Comparison with other red quasars

Our ISPI NIR photometry reveals that for our slightly extended system some flux is missed when measured via the (default) point–source photometry of 2MASS (Tab. 1). More appropriate is the 2MASS aperture photometry (4″aperture), which includes both objects. It agrees well with our new photometry which in turn reduces the colour of the quasar alone from 1.95 to  1.5 (Tab. 1). The flux ratio of J2341 to its companion is similar in , , and , while it significantly different in . This indicates that both objects are dominated by a comparable old stellar population at red optical to NIR wavelengths. In this case their colour should also be the same. We attribute the 0.6 mag increase in in the quasar to additional hot dust emission. This also indicates that the central regions of the quasar are not severely obscured which otherwise would affect the NIR emission.

The colour of J2341 is bluer than the threshold used to select the 2MASS red AGN (; Cutri et al. (2002)) which show various optical continuum slopes (e.g. Smith et al. (2003)) and X–ray properties (e.g. Wilkes et al. (2002)). For the 2MASS red AGN we most likely observe a range from essentially unobscured to absorbed sources. The red colour can then be attributed to either clearly visible emission from hot dust in the centre or to absorption of the continuum.

In the picture where nuclear activity is triggered by interaction red quasars are supposed to represent young members of the QSO population. While so far only a moderate fraction of 2MASS red AGN and classical blue PG quasars show signs for interaction on HST images (; Marble et al. (2003)), J2341 clearly has a spectroscopically confirmed companion (Fig. 3).

4.4 On the origin of the red quasar continuum

We now discuss the faint optical continuum emission of J2341, which is unusual for optically selected type-1 QSOs. The aim is to see how far common mechanisms are able to explain the nature of J2341.

First, we assume that J2341 has an intrinsically blue continuum similar to the SDSS quasar template from Vanden Berk et al. ((2001)), but that J2341 is reddened by a dust screen (Sect. 4.4.1) and in addition diluted by stellar light of the host galaxy (Sect. 4.4.2).

It should be noted that the SDSS template is quite similar to other QSO composites like those from the Large Bright Quasar Survey or the First Bright Quasar Survey (Fig. 11 in Vanden Berk et al. (2001)). The relative spectrum–to–spectrum variation of the quasars forming the SDSS template is about 15–20% in the wavelength range 3000–5000  (Fig. 10 in Vanden Berk et al. (2001)), hence relatively small. The power–law slope between Ly and H is somewhat redder for a composite formed from quasars (; ) than the slope for the entire quasar sample entering the SDSS template (). But this effect is small for the wavelength range considered here, i.e. compared with template from the entire sample, the redder slope of the template reduces the 3000  continuum by only 10%, when keeping the 4863  flux fixed. Therefore, we here use the SDSS template from the entire sample, assuming that it represents an essentially unreddened quasar spectrum. Furthermore, the SDSS template still contains contributions from the host galaxy (especially at red optical wavelengths), hence for a reasonable comparison any host contributions in J2341 will rather tend to make the differences to the SDSS template smaller than larger.

Since these two mechanisms – dust screen reddening and dilution by the host galaxy – do not fully explain the red nature of J2341, we discuss further scenarios in Section 4.4.3.

Filter 2MASS 2MASS ISPI QSO/comp nuclear/total
(1) (2) (3) (4) (5) (6)
17.52 18.02 3.0 0.34
16.505 16.065 16.01 3.1 0.35
15.502 15.234 15.21 3.3 0.42
14.555 14.577 14.49 5.5 0.44
Table 1: Photometry of the J2341 system, given in Vega magnitudes. The errors of the NIR photometry are mag. (2) Default 2MASS PSF photometry includes both objects. The –mag is taken from USNO–B. (3) 2MASS 4″aperture photometry. (4) ISPI aperture photometry, –mag taken from the VLT acquisition frame. (5) Peak flux ratio of quasar-to-companion from nuclear (1″) gaussian fitting. (6) Fraction of total flux contained in nuclear gaussian fits (quasar + companion); the complementary flux is due to extended emission.

Dust screen reddening

In numerous cases it has been shown that the spectra of luminous red quasars can be matched with template spectra quite well if simple dust screen reddening is applied (e.g. quasars from the FIRST-2MASS survey, Gregg et al. (2002)). This technique works also well for low– AGN where host galaxy contributions become important. For example, one nearby red type–1 QSO from the Spitzer First Look Survey (SSTXFLS J171335.1+584756 at ; Lacy et al. (2007)) shares some basic properties with J2341: FLS J1713 has a red optical continuum, broad Balmer emission lines (although narrower than in J2341), and Ca II absorption lines indicating contributions from the host galaxy. However, between 24 m and 70 m the SED of FLS J1713 looks more like that of the ULIRG-AGN Mrk231, with a 70 m / 24 m flux ratio of about 4. As a test we reddened the SDSS template using SMC dust extinction curves (Gordon et al. (2003)) to match the spectrum of FLS J1713. The rest–frame continuum is decently represented between and by the SDSS template reddened with E (shortwards of = no spectral data are available). This test demonstrates that even some nearby red quasars (which include host galaxy emission) can be explained by simple screen reddening of optical QSO templates, at least longward of = .

Figure 5 shows the spectrum of J2341 and the unreddened SDSS QSO template. The spectra are scaled to match in the H line. This highlights the difference in the optical continua of J2341 and the template. It suggests reddening in J2341 bluewards of which becomes particularly strong for .

After applying a dust screen reddening of E to the template both spectra match well down to (Fig. 7, top). Also, the fluxes of the broad H and H lines match for both spectra. This shows that a dust screen of E accounts pretty well for reddening on sightlines towards the broad–line region of J2341 (assuming the same intrinsic Balmer ratio). We determined the uncertainty of the spectral matching to .

However, shortwards of J2341 still lacks significant continuum flux compared to the reddened template (Fig. 7, top). At the discrepancy is about a factor 3. An E would be necessary to match the blue part of the template with the observed J2341 spectrum (Fig. 7, bottom). But with E we already have accounted for the amount of dust towards the centre as traced by the broad emission lines. If a reddening of E was indeed present towards the central regions of J2341 the intrinsic H / H would be which is not supported by either theory (e.g. Kwan (1984)) or observations (e.g. Shang et al. (2007)). Therefore, other explanations than extinction by a dust screen have to be considered to account for the remaining difference at blue optical wavelengths.

Figure 7: Comparison of the spectrum of J2341 with the SDSS quasar template moderately reddened E (top), and strongly reddened E (bottom).

Dilution by host galaxy light

An underlying host galaxy with a pronounced 4000 Å break can in principle dilute the signature of the blue bump emission, i.e. the rising blue continuum.

We note that QSO templates – especially at red optical wavelengths – are dominated by emission from local, lower luminosity AGN and, thus, a significant host galaxy component may already be included (e.g. Vanden Berk et al. (2001); Gaskell et al. (2004)). On the other hand, for blue optical wavelengths higher redshift (and higher luminosity) sources dominate the template and the influence of the host galaxy on the overall spectral shape of the template is reduced.

Since the subtraction of several template galaxy spectra taken from the literature (e.g Calzetti et al. (1994); Kinney et al. (1996)) give poor results we therefore extracted the host galaxy spectrum directly from our two dimensional spectral frames (see also Bennert et al. (2006)). This results in a much better fit to the absorption features in the QSO, even considering the moderate S/N of the host spectrum.

The host spectrum was extracted from an area of 08 with a separation of 1″ south–east (3.7 kpc) to the region of the QSO spectrum (Fig. 1). The placement and width of the region used for the host spectrum extraction was chosen to provide maximal S/N without contamination from nuclear QSO light. The host spectrum shows clear Ca II H+K absorption as well as [O ii] and narrow H/[N ii] emission (Fig. 8, top). For the same reasons as for the companion spectrum we expect the stellar template to be largely free of AGN contamination (no broad–line components, no high–ionisation lines; see § 3). While the [O ii], H, and the weak [O iii] emission could result from an extended narrow–line region, it can also indicate ongoing star formation in the host galaxy. The flux ratio of F suggests star formation as cause for the line emission in the host galaxy.

Following Boroson et al. ((1982)) we also obtained a host galaxy spectrum by subtracting the nuclear 06 spectrum from a spectrum of 30 width which covered the quasar plus host emission (on the opposite side from the companion). The nuclear spectrum was scaled in such a way that the broad lines were removed and only the underlying host galaxy spectrum remained. This spectrum agrees very well with the spectrum from the off–nuclear extraction supporting our approach. In the further analysis only the off–nuclear spectrum was used.

Figure 8: The extracted host spectrum without (top) and with additional reddening of E ontop of the QSO spectrum (dashed line). The host spectra are scaled to remove the Ca II K feature from the QSO after subtraction. Just for these graphs additional offsets were applied to the host spectra to facilitate an easy comparison with the QSO.

We scaled the host spectrum in such a way that, after subtraction from the QSO spectrum, the Ca II K line is removed. We also tried other scalings but even the most extreme values explored were not able to recover the blue bump emission while on the other hand highly overestimating the Ca II K absorption. Thus, we used the Ca II K line as a measure for the host galaxy contribution.

This subtraction also recovers the H line in a reasonable strength (Fig. 9, top). This line was largely absent in the original spectrum due to the underlying Ca II H absorption. Down to about 4500  the resulting “host–free” QSO spectrum of J2341 fits the dust reddened SDSS QSO template better than the original J2341 spectrum does. But shortwards of 4500  the “host–free” J2341 system still lacks continuum, and at 3000  the discrepancy is about a factor of 2. This is too large to be explained by the 10–20% spectrum-to-spectrum variation of the SDSS template or the 10% redder slope of the template. Even if a redder template made of extraordinarily UV–weak quasars would fit J2341 better, it is of particular interest to explore the nature of such potentially UV–weak quasars.

Figure 9: Comparison of the moderately reddened SDSS quasar template with the spectrum of J2341 after subtraction of the host without reddening (top), and with additional reddening (bottom).

A refined way to account for the remaining discrepancies between the QSO template and the J2341 spectrum would be to consider increased reddening towards the centre of the system, as found by e.g. Bennert et al. ((2006)) for their Seyfert galaxies. Then the nuclear host galaxy component, as seen in the J2341 QSO spectrum, would be more reddened than the extracted host galaxy template 3.7 kpc further out. Reddening of the host galaxy spectrum before subtraction from the QSO gives an interesting results (Fig. 8, bottom): After applying a redding equivalent to E the reddened host galaxy spectrum follows the spectral shape of the QSO remarkably closely. (We chose E since that was the value inferred as reddening towards the broad–line region.) Due to the similarity in spectral shape the subtraction of the reddened host galaxy spectrum from the QSO results in the QSO spectrum being almost flat in flux over the observed wavelengths (Fig. 9, bottom). This makes the fit of the J2341 spectrum with the SDSS QSO template worse over almost the whole wavelength range compared to the case with an unreddened host galaxy.

It is also possible that the stellar population in the centre differs from that at a few kiloparsec further out. But Bennert et al. ((2006)) found this issue to be only of minor importance for their spatially well resolved object (NGC 1386).

To summarise, so far the comparison with the SDSS quasar template strongly suggest that dust screen reddening alone and the combination of screen reddening with host galaxy contributions are not able to fully explain the red optical/UV continuum of J2341 shortwards of H. Therefore, we consider alternative scenarios.

Refined scenarios and alternatives

In this section we discuss special dust distributions and other effects. So far we have applied a dust screen of E to the SDSS template in order to match its spectrum with J2341 after subtraction of the host. The dust cannot be distributed evenly throughout the whole galaxy, because we clearly detect features of the host galaxy in the optical spectrum of the quasar, while the AGN continuum appears heavily suppressed (Fig. 4). Moreover, the emission lines from the NLR are still clearly visible in J2341 suggesting that the major part of the obscuring material is located in the centre of the galaxy, somewhere between the NLR and the accretion disc (e.g. Fig. 4).

Small, sharply confined dust clouds with a low volume filling factor may lie by chance in our line of sight towards the accretion disk, which produces the continuum emission. Then the clouds may redden the AGN continuum emission, while the bulk of the slightly more extended BLR may be less affected. This scenario appears in accordance with results from X–ray spectroscopy of red 2MASS type– 1 AGN, where the presence of a compact absorber very near to the active nucleus has been proposed. In these AGN the BLR is clearly visible, but the X–ray source is significantly obscured (e.g. Wilkes et al. (2005)). We should note, however, that the X–ray absorption traces the gas while the optical obscuration is due to dust. In addition, if a low volume filling factor is assumed, the swirling dust clouds are expected to shield the centre not permanently (transient shielding). Hence, we expect significant variability in both the total intensity and the spectral shape. But we detect neither a significant difference in the spectral slope of our spectra (that span two years) nor are significant photometric differences observed by comparison of SDSS and USNO–B data (that span 40 years).

Another explanation considers that light from the nucleus grazes the edge of a moderately inclined torus so that the BLR is largely seen, but the accretion disk is essentially hidden and strongly reddened (see also Smith et al. ((2004)) who proposed a similar scenario to explain the polarisation properties of a group of Seyfert 1 galaxies). Then the torus must have a rather sharp edge, a requirement which looks unlikely because the ongoing interaction favours a more disturbed dust distribution. In addition, the MIR spectra do not show recognisable silicate absorption placing an upper limit on the MIR absorption and, thus, on the optical absorption of A 1 (following Krügel et al. (2003)). This upper limit is consistent with our finding of E. Therefore even this special geometry does not provide a satisfying explanation for substantially higher extinction towards the accretion disk.

Next we discuss screen versus mixed case reddening. Simple screen reddening by dust is not suitable to explain simultaneously the reddening of the BLR and the continuum. But dust mixed with the BLR may be in accordance with the observations. Then the BLR suffers only moderate mixed case reddening, while the continuum is more strongly reddened by the entire absorbing screen. However, this requires dust inside the dust sublimation radius mixed with the BLR, where it should ultimately be destroyed by the strong radiation field of the nucleus.

Since common mechanisms fail to provide a satisfying explanation for the red continuum of J2341, it seems that the strong Blue Bump emission of average quasars is largely missing in J2341. For low–luminosity AGN (LLAGN) radiatively inefficient accretion flows (RIAFs) were proposed to explain the lack of prominent Big Blue Bump emission in the UV (e.g. Ho (1999); Narayan (2005)). Although J2341 qualifies as a bona fide quasar from its luminosities at different wavelengths, the spectral shape towards the UV is reminiscent of RIAFs. Since the dust models have difficulties to consistently explain the spectrum of J2341, the RIAF scenario is an attractive possibility to interpret the observations. However, the detection of prominent high excitation lines like [Ne v] strongly questions an intrinsically low UV flux.

Even the refined scenarios have difficulties matching J2341 with standard blue quasar templates. This leads us to suggest that the continuum of the quasar J2341 is intrinsically redder than that of typical quasars, although not being in a RIAF phase.

Since the enigmatic UV–weak nature of J2341 may also be found in other objects further studies of this prototypical object are desired.

Higher S/N data in which several stellar absorption features are securely identified could allow for a more detailed way to account for the host galaxy contribution. On the other hand, observations in the rest–frame UV range would be especially interesting for the apparent lack of a prominent Small Blue Bump while strong Balmer and Fe ii emission is observed in the optical. Studies sampling this wavelength range are needed to further address this phenomenon.

Acknowledgements.
Part of this work was supported by Sonderforschungsbereich SFB 591 “Universelles Verhalten gleich-gewichtsferner Plasmen” der Deutschen Forschungsgemeinschaft, and by Nordrhein–Westfälische Akademie der Wissenschaften. We thank Dan Weedman for kindly providing the Spitzer spectrum of Mrk 231. We also thank Andy Robinson for his helpful comments on the manuscript. Based on observations with the Infrared Space Observatory ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and UK) and with the participation of ISAS and NASA. The Two Micron All Sky Survey is a joint project of the University of Massachusetts and IPAC/Caltech, funded by the National Aeronautics and Space Administration and the National Science Foundation.

Footnotes

  1. thanks: Based on observations made with ESO Telescopes at La Silla and Paranal under programme IDs 275.A-5064 and 075.A-0374, with the Spitzer Space Telescope, which is operated by the JPL, CALTECH under a contract with NASA, and obtained at CTIO a division of NOAO, which is operated by AURA under cooperative agreement with the National Science Foundation.

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