Looking for blazars in a sample of unidentified high-energy emitting Fermi sources

Looking for blazars in a sample of unidentified high-energy emitting Fermi sources

Key Words.:
Gamma rays: general – X-rays: general – galaxies: active – (galaxies:) BL Lacertae objects: general


Context:Based on their overwhelming dominance among associated Fermi –ray catalogue sources, it is expected that a large fraction of the unidentified Fermi objects are blazars. Through crossmatching between the positions of unidentified –ray sources from the First Fermi Catalog of –ray sources emitting above 10 GeV (1FHL) and the ROSAT and Swift/XRT catalogues of X–ray objects and between pointed XRT observations, a sample of 36 potential associations was found in previous works with less than 15 arcsec of positional offset. One-third of them have recently been classified; the remainder, though believed to belong to the blazar class, still lack spectroscopic classifications.

Aims:We study the optical spectrum of the putative counterparts of these unidentified gamma-ray sources in order to find their redshifts and to determine their nature and main spectral characteristics.

Methods:An observational campaign was carried out on the putative counterparts of 13 1FHL sources using medium–resolution optical spectroscopy from the Osservatorio Astronomico di Bologna in Loiano, Italy; the Telescopio Nazionale Galileo and the Nordic Optical Telescope, both in the Canary Islands, Spain; and the Observatorio Astronómico Nacional San Pedro Mártir in Baja California, Mexico.

Results:We were able to classify 14 new objects based on their continuum shapes and spectral features.

Conclusions:Twelve new blazars were found, along with one new quasar and one new narrow line Seyfert 1 (NLS1) to be potentially associated with the 1FHL sources of our sample. Redshifts or lower limits were obtained when possible alongside central black hole mass and luminosity estimates for the NLS1 and the quasar.

1 Introduction

The most important objective of the Fermi mission is to study the whole sky at –ray energies; this is achievable with the use of the Large Area Telescope (LAT) thanks to its large collecting area and field of view (Atwood et al., 2009). The location accuracy of the telescope, which detects –ray objects emitting at GeV energies, is between 0.5 to 10 arcminutes, depending on the source detection significance.

There are more than 3000 sources listed in the latest release of the Fermi catalogue (Acero et al., 2015). Of these, only 238 are considered firm identifications by the LAT team, based on spatial morphology, correlated variability, and/or periodic lightcurve properties. Another sources have high confidence associations, based on cross-correlations with multiwavelength catalogues. The majority of these identified and associated sources belong to one of the following categories: extragalactic objects such as blazars (flat spectrum radio quasars or BL Lacs), or Galactic sources (mainly pulsars, pulsar wind nebulae, and supernova remnants). However, there is still an important number of sources (about 30%) without proper identification, i.e. lacking association with any known class of –ray emitting objects, which constitute the class of unidentified/unassociated gamma-ray sources (UGSs).

A similar but less critical situation is found when considering the First Fermi Catalog of detected sources above 10 GeV (1FHL; Ackermann et al., 2013): from a total of 514 listed sources, 65 (13%) are UGSs. These are also the numbers resulting from analysing the Second Fermi Catalog of detected sources above 50 GeV (Ackermann et al., 2016, 2FHL;): it lists 360 sources, of which 48 (14%) are UGSs.

The search for counterparts of these new high–energy sources is hindered by the relatively large (in comparison with longer wavelengths) Fermi positional error ellipses. This uncertainty in their location means that positional correlations with known objects is often not enough to identify a Fermi source; thus, a multiwavelength approach is needed in order to understand their nature, using X–ray, optical and radio data of likely counterparts. X–ray data analyses are particularly useful in finding a positionally correlated object with broadband spectral parameters that might be expected in a –ray emitting source. Soft X–ray surveys (i.e. with energies below 10 keV) are convenient for this task because they offer 3 great advantages: They cover the whole Fermi error ellipse, their positional accuracy is of the order of arcseconds, and they provide information in an energy band close to that at which the Fermi LAT operates. Since most of the 1FHL sources are BL Lacs and in particular high-energy cutoff BL Lacs (HBL), and as they show the peak of the SED synchrotron component in the X-rays, crossmatching the Fermi catalogue with X-ray surveys should prove useful as a tool to select them. This allows the positional uncertainty of the objects detected with Fermi to be restricted, thus facilitating the identification process.

To this end, following Stephen et al. (2010), Landi et al. (2015a, b, c) performed a crossmatch between the positions in the 1FHL catalogue, the ROSAT All–Sky Survey Bright Source Catalogue of sources detected between 0.1–2.4 keV (Voges et al., 1999) , the 1SXPS Catalogue of X–ray sources detected with Swift/XRT in the 0.3-–10 keV band (Evans et al., 2014), and pointed XRT observations available at the ASI Science Data Center1 archive. They found correlations with a strong level of confidence (), leading to evidence for the potential association of a number of UGSs with X–ray counterparts, improving the positional error in all correlated objects, and thus opening the possibility for optical follow–up.

In particular, 36 secure 1FHL/X–ray potential associations were obtained which allowed the selection of a likely low–energy (optical and below) counterpart for all of them. An investigation of the nature of these sources on the basis of their archival multiwavelength properties indicates that all potential associations are either recently identified blazars (Landi et al., 2015c; Landoni et al., 2015; Massaro et al., 2015b; Ricci et al., 2015) or blazar candidates (Landi et al., 2015b, a). The majority of blazars are expected to show –ray emission in the GeV range (e.g. Acero et al., 2015). Nevertheless, 24 of the potential 36 associations are still lacking an optical spectroscopic confirmation of their nature.

According to Stephen et al. (2010) and Landi et al. (2015b), 1FHL sources like these can be responsible for the emission of very high energy –rays, up to the teraelectronvolt (TeV) range (Padovani & Giommi, 1995; Fossati et al., 1998). The interest in extreme TeV blazars arises from the possibility of obtaining information on both the acceleration processes of charged particles in relativistic flows (e.g. Ghisellini et al., 2010) and the intensity of the extragalactic background light (e.g. Georganopoulos et al., 2010), which reflects the time–integrated history of light production and re–processing in the universe, and hence its measurement can provide information on the history of cosmological star formation (Mankuzhiyil et al., 2010). This is important when considering that in the 1FHL catalogue, only 22 (%) objects of the AGN type are considered to be firmly identified out of a total of 393 cases (Ackermann et al., 2013). This is why the confirmation of the nature of even a small subset of the unidentified objects of the 1FHL sample would significantly increase the statistics of the GeV/TeV emitting blazars class, which in turn is only achievable after finding the proper association. This would also be relevant for a future search of TeV blazars that can be performed with the Cherenkov Telescope Array (Massaro et al., 2013b).

Furthermore, as the number of detected sources in the high–energy surveys is growing at an ever–increasing speed, it is necessary to establish well–defined methods to correctly identify and classify as many objects as possible while strictly reducing their positional uncertainties. Therefore, the aim of this work is to spectroscopically analyse 14 optical targets with near-positional coincidence with the X–ray sources out of those 24 without classification. Following the treatment of Stephen et al. (2010), we expect no more than only one spurious correlation out of the selected sample of 14 objects.

Number USNO designator RA(J2000) DEC(J2000) Observatory UT date Time Total exp.
X-ray association [mm/dd/yy] [mid. exp.] [s]
(1) (2) (3) (4) (5) (6) (7) (8)
1 U0750-00173701 NOT 10/13/2015 1200
1RXS J004349.3-111612
2 U0975-00792795 NOT 10/13/2015 1200
1SXPS J033829.0+130213
3 U0675-01653184 NOT 10/13/2015 1200
1SXPS J043949.5-190102
4 U0750-02519189 NOT 10/13/2015 1200
1SXPS J064007.1-125313
5 U0875-0218538 NOT 10/14/2015 1200
1SXPS J074627.1-022550
6 U0825-05946383 LOI 03/10/2015 3600
1RXS J080458.3-062432
7 U0825-05946383 SPM 01/14/2016 1800
SWXRT J111515.3-070126
8 U0750-08080787 LOI 03/13/2015 3600
1SXPS J131553.0-073301
9 U1575-03416792 TNG 08/26/2015 2400
1SXPS J141045.3+740508
10 U1575-03416943 TNG 08/26/2015 1200
1SXPS J141051.3+740410
11 U0600-17715078 TNG 08/27/2015 2000
1RXS J151213.1-225515
12 U0825-08948904 TNG 08/27/2015 2400
1SXPS J154952.1-065908
13 U1125-10089754 TNG 08/27/2015 1600
1RXS J184121.8+290932
14 U1530-0317394 TNG 08/29/2015 3600
1RXS J200245.4+630226
Table 2: We report the name in the USNO and X–rays catalogues in column 2, in columns 3 and 4 coordinates referring to J2000.0 for each optical target, in column 5 the observatory, in column 6 the date of observation, in column 7 the UT time at mid exposure, and in column 8 the total exposure time in seconds for each of the optical pointings.
Table 1: Observed sample of unidentified sources from the 1FHL catalogue.

In the following sections, we describe our optical follow–up work on a subsample of 14 of the aforementioned potentially associated objects from the 1FHL catalogue. From these, only 1FHL J1549.9-0658 appears in the 2FHL catalogue (named 2FHL J1549.8-0659), although there is also a detection positionally consistent (2FHL J0639.9-1252, at a distance of arcmin) with 1FHL J0639.6-1244. The reason why only one of the 1FHL objects from our sample can be found in the 2FHL catalogue is the energy threshold: The 2FHL catalogue includes only those sources detected at 50 GeV or more, while the 1FHL catalogue has a threshold of 10 GeV.

We note that 1FHL J1410.4+7408 shows two different X–ray objects (Landi et al., 2015b) within its –ray positional error box, each with a single corresponding optical source. We define 1FHL J1410.4+7408 A as the one marked as #1 in Landi et al. (2015b), and 1FHL J1410.4+7408 B as the one marked as #2. In section 2 we briefly discuss the selection of the sample, in section 3 we describe the observations, in section 4 we analyse our results, and in section 5 we summarise our conclusions.

2 Sample selection

Our sample of 1FHL fields is a subset of those presented in Landi et al. (2015a, b).

They found only one X–ray counterpart for each Fermi source, with the exception of 1FHL J1410.4+7408. However, despite the better positional accuracy achieved, it is important to note that X–ray error circles are still large enough (i.e. 6 arcseconds) to find more than one optical source tentatively associated with each single X–ray counterpart. Thus, a supplementary investigation is needed to single out the actual counterpart of the –ray/X–ray emitter. For this reason, we set up an international campaign to obtain spectroscopic observations of candidate optical counterparts in 13 fields, which are the subject of this paper. Details on the observations can be found in Table 1.

3 Observations

The optical spectroscopic observations were carried out at four different observatories for a total of 18 nights:

  • Three nights (from 10 Mar 2015 to 12 Mar 2015) at the 1.52m Cassini telescope of the Bologna Observatory in Loiano (LOI), Italy, with the BFOSC spectrograph and a 2.0 arcsec slit (0.40 nm/px dispersion). The data covered a range from 350 to 800 nm.

  • Three nights (19 May 2015, 21 Jun 2015, and 09 Jul 2015) at the 3.58m Telescopio Nazionale Galileo (TNG) in La Palma, Canary Islands, Spain, with the DOLORES (LRS) spectrograph and a 1.5 arcsec slit (0.25 nm/px dispersion). The data covered a range from 370 to 800 nm.

  • Two nights (13 Oct 2015 and 14 Oct 2015) at the 2.5m Nordic Optical Telescope (NOT), in La Palma, Canary Islands, Spain, with the ALFOSC spectrograph and a 1.0 arcsec slit (0.30 nm/px dispersion). The data covered the 350 to 900 nm range.

  • Eight nights (from 06 Nov 2015 to 09 Nov 2015 and from 14 Jan 2016 to 17 Jan 2016) at the 2.12m telescope in San Pedro Mártir (SPM), Mexico, with the Boller & Chivens spectrograph and a 2.5 arcsec slit (0.23 nm/px dispersion). The data covered a range from 350 to 800 nm.

The data were cleaned from cosmic rays, bias corrected, flat–fielded, and both wavelength and flux calibrated using IRAF2 standard packages, wavelength calibration lamps, and spectrophotometric standard stars. In each case, the estimated wavelength calibration error is less than 0.4 nm.

4 Results

In Figure 1, we present the optical spectra for each analysed object in the upper panels, while in the lower panels we show the continuum–normalised spectra in order to highlight the presence of spectral features (if any).

Figure 1: Optical spectra obtained for the whole sample presented in this paper. Upper panels show the observed spectra, while lower panels show the spectra with normalised flux. Absorption lines or bands present at 686.9 nm, 718.6 nm, and 760.5 nm are telluric. Absorption lines present at 589.0 nm and 589.6 nm correspond to the NaI doublet from the interstellar medium, although in the case of 1FHL J0639.6-1244 it could possibly be superimposed on the MgI line at . Lines marked ’DIB’ correspond to diffuse interstellar bands, while those marked with a question mark are hard to identify because they are on the edge of detection and because of the lack of other lines to obtain a redshift value. Sources are given with their USNO designator, while the proposed 1FHL counterpart is given in parenthesis.
Figure 1: (Continued).
USNO designator Features EW [Å] Flux Redshift Class
1FHL association (Distance)
(1) (2) (3) (4) (5) (6)
U0750-00173701 BL Lac
1FHL J0044.0-1111 (5.7)
U0975-00792795 BL Lac
1FHL J0338.4+1304 (2.5)
U0675-01653184 BL Lac
1FHL J0439.9-1858 (2.9)
U0750-02519189 G 1.00.6 -8-4 0.1350.001 BL Lac
1FHL J0639.6-1244 (10.7) Na 2.31 -21-10
U0875-0218538 BL Lac
1FHL J0746.3-0225 (1.7)
U0825-05946383 BL Lac
1FHL J0804.8-0626 (2.1)
U0825-05946383 Ly 31228 9510 2.9290.003 QSO
1FHL J1115.0-0701 (3.2) NV 26249 7612
SiV/OIV 7914 213
CIV 26431 826
U0750-08080787 BL Lac
1FHL J1315.7-0730 (3.3)
U1575-03416792 MgII 176 154 0.4290.001 NLS1
1FHL J1410.4+7408 A (4.4) H 189 94
H 3514 145
U1575-03416943 BL Lac
1FHL J1410.4+7408 B (3.3)
U0600-17715078 BL Lac
1FHL J1512.1-2255 (1.0)
U0825-08948904 BL Lac
1FHL J1549.9-0658 (1.4)
U1125-10089754 BL Lac
1FHL J1841.1+2914 (5.6)
U1530-0317394 FeII 117 -1.5-0.9 0.9 BL Lac
1FHL J2002.6+6303 (1.1) MgIIa 103 -1.6-0.6
MgIIb 72 -1.1-0.4
Notes: The units for all the reported flux densities are .
The equivalent width (EW) is given in the observer’s frame. Emission lines are given
as positive flux values, and absorption lines as negative flux values. The distance
between the USNO source and the 1FHL centroid is given in arcseconds.
Table 3: Nature of each of the observed optical counterpart candidates for 1FHL sources.

In 12 out of 14 cases, the spectra resulted in non-thermal continua. Moreover, no intrinsic features were present in 10 out of 14 objects. Both are typical characteristics of blazar spectra. In all cases in which some features are found, a redshift (or at least a lower limit to it) was derived, in addition to obtaining equivalent widths and fluxes for all lines, in order to determine the nature of each source. Results from our analysis can be found in Table 3, where we report in column 1 the USNO source name along with the name of the proposed 1FHL counterpart and the distance between them, in column 2 the emission and/or absorption lines found (if any), in columns 3 and 4 their measured equivalent widths and fluxes, in column 5 the derived redshift (if any), and in column 6 the classification of the source. Further details are shown in the next sections.

It is worth mentioning that, in the cases of 1FHL J1115.0-0701 and 1FHL J0804.8-0626, the correlation with X–ray data showed only one source inside the –ray positional error area, while in optical wavelengths (as seen in the USNO plates, with a limiting magnitude of mag) two objects could be found within the X–ray error circle. In both cases, the other object was also analysed and ruled out because of its star–like spectrum, i.e. showing a thermal continuum, no emission lines, and a variety of absorption lines potentially associated with stellar processes (for instance, the Balmer series) at redshift zero. A different case is that of fields 1FHL J1410.4+7408 A and B, which are potentially associated with the same source in the 1FHL catalogue but for which two X–ray objects were found within the –ray error ellipse (Landi et al., 2015b) and, consequently, two putative optical counterparts could be potentially associated with this –ray source. This case will be discussed in Section 5.2.

Once confirmed as potential counterparts (i.e. after discarding all the sources from which no high-energy emission is expected, as for example stars), we improved their equatorial coordinates by searching for detected objects in the 2MASS (Skrutskie et al., 2006) catalogue, which provides positions with uncertainties of less than 0.1 arcsec. Only four of them were not found in this catalogue: the optical sources potentially associated with 1FHL J1410.4+7408A, 1FHL J1410.4+7408B, 1FHL J1549.9-0658, and 1FHL J1841.1+2914. Nevertheless, the first three were found in the USNO-A2.0 catalogue (Monet, 1998), and the last one in the USNO-B1.0 catalogue (Monet et al., 2003), which provide an accuracy of 0.2 arcsec.

Source details are given in the following subsections.

4.1 BL Lacs

Out of the 14 optical sources observed, we were able to classify 12 as blazars of BL Lac class: These are our associations with Fermi sources 1FHL J0044.0-1111, 1FHL J0338.4+1304, 1FHL J0439.9-1858, 1FHL J0639.6-1244, 1FHL J0746.3-0225, 1FHL J0804.8-0626, 1FHL J1315.7-0730, 1FHL J1410.4+7408 B, 1FHL J1512.1-2255, 1FHL J1549.9-0658, 1FHL J1841.1+2914, and 1FHL J2002.6+6303. Indeed, all the sources show a non–thermal, power–law, intrinsically blue continuum, and no apparent intrinsic emissions or absorptions, with the exception of U0750-02519189 (associated with 1FHL J0639.6-1244), in which its host galaxy contribution is visible (meaning it is a blazar of the BZG type, as described by the Roma-BZCAT catalogue in Massaro et al. (2015a)), showing Na and G-band absorptions at a redshift . This, alongside a lower limit for the redshift of our association for 1FHL J2002.6+6303, U1530-0317394 (), obtained from the detection of intervening FeII and MgII absorptions, is the only value for we were able to derive from the spectra of this BL Lac subsample.

In the case of the optical association of 1FHL J0804.8-0626, there are two optical sources inside the X–ray error box, according to the USNO plates. Both of them were observed and analysed. The faintest one (at optical position ) showed a normal G-type star spectrum, thus discarding any possibility of potential association with the high–energy emitting source. The coordinates published in Table 2 are thus those of the BL Lac conclusively associated through optical spectroscopy, which is the WISE source suggested by Landi et al. (2015a) and which we associate with the –ray source.

4.2 U1575-03416943

This source potentially associated with 1FHL J1410.4+7408 A shows clear emission lines (MgII, H, H, H, and [OIII]) at a common redshift . Given that the velocities associated with the emission of the H line are around , and that the ratio between the fluxes of emission lines and is , we conclude that this object is a narrow line Seyfert 1 galaxy (NLS1, Osterbrock & Pogge, 1985; Goodrich, 1989).

4.3 U0825-05946383

The field associated with 1FHL J1115.0-0701 presented two optical sources within the X–ray positional uncertainty box, according to the USNO plates. In this case, again, both spectra were analysed, and we could discard one of them on the basis of typical stellar features (in particular, we classified it as a K-type star, at position ).

The spectrum of the other optical source shows strong, luminous emission lines for Ly, NV, SIV, and CIV, at the high redshift value of ; these characteristics are typical of a high–redshift quasar. However, its potential association with the 1FHL source is not ironclad (see Section 5.3).

5 Discussion

In this section we analyse in detail the spectral characteristics of the results obtained for the 14 objects we spectroscopically associated in this work. In particular, we discuss general properties in subsets divided by class of object: BL Lacs (12 objects), NLS1 (1 object), and quasars (1 object).

5.1 BL Lacs

In order to analyse the emission processes involved, we built a plot of spectral indices as shown in Abdo et al. (2010), which is useful to easily spot the synchrotron peak for each object. To this end, and following Masetti et al. (2013), we searched for the X–ray fluxes of the sources in our sample as measured with XRT or ROSAT, corrected from Galactic absorption with PIMMS (Mukai, 1993) using the Galactic values given by Landi et al. (2015b), when available, or those given by Kalberla et al. (2005). We also retrieved their magnitudes from the USNO catalogues, from which we derived absorption-corrected fluxes using the absorption maps from Schlegel et al. (1998), the reddening law of Cardelli et al. (1989), and the total-to-selective extinction ratio of Rieke & Lebofsky (1985); with the conversion factor of Fukugita et al. (1995) we then rescaled the flux values to 500 nm using the same procedure given by Masetti et al. (2013). Furthermore, we obtained their radio flux densities at 1.4GHz, when available, from the NVSS catalogue (Condon et al., 1998) and rescaled them to 5 GHz assuming a radio flat spectral shape (Begelman et al., 1980) in order to use the same relationship given in Abdo et al. (2010).

With the radio, optical, and X-ray absorption-corrected fluxes we were able to obtain spectral indices from X–ray to optical and from optical to radio frequencies. In Figure 2, we included all the sources from this sample, numbered in order of right ascension (see Table 2), in a plot (Padovani & Giommi, 1995; Abdo et al., 2010). In dashed lines, we indicate the location of synchrotron peaks at low (), intermediate (), and high () frequencies. Eight BL Lacs in our sample have their synchrotron peaks at a frequency higher than , which are likely candidates to be detected at TeV energies (Massaro et al., 2008). It is important to highlight that the BL Lac associated with 1FHL 1410.4+7408 B did not show any radio emission, which is why we used the detection threshold from the NVSS survey () as upper limit to its radio flux density. The resulting lower limit to is indicated in the plot with an arrow.

For completeness, we also included the recently studied optical objects associated with 1FHL J1129.2-7759, 1FHL J1328.5-4728, and 1FHL 2257.9-3644 which were confirmed as BL Lacs by Massaro et al. (2015b) (for which we found an intermediate synchrotron peak, marked with an M in Figure 2), Ricci et al. (2015) (which shows a low synchrotron peak, marked with an R) and Landoni et al. (2015) (intermediate synchrotron peak, marked with an L), respectively. These objects are also part of the sample selected by Landi et al. (2015a) and Landi et al. (2015b). In addition, we added the two non-BL Lac objects from our sample, the potential associations with 1FHL J1410.4+7408 A (the NLS1 presented in Section 4.2) and 1FHL J1115.0-0701 (the quasar) just to present the whole sample in one plot, although it is not possible to compare these sources with BL Lacs given that this kind of objects generally present a thermal emission component which cannot be easily separated from the non-thermal one. Neither one presents radio emission, as seen in Figure 2, so also in this case we used the NVSS threshold value to determine a lower limit for .

Figure 2: Analysed sources in the spectral indices plane. Lower limits are indicated with an arrow. Numbers refer to the values presented in Table 2, while letters L, M, and R refer to the objects in Landi et al. (2015b, a) associated by Landoni et al. (2015), Massaro et al. (2015b), and Ricci et al. (2015), respectively. Sources 5, 6, 11 and 13 are shown as points for the sake of clarity. The red shaded area indicates the region where the relationship describing synchrotron peak values changes its functional form, as explained in Abdo et al. (2010).

5.2 The case of 1FHL J1410.4+7408

As 1FHL J1410.4+7408 is potentially associated with two different X–ray emitting and optically peculiar objects according to Landi et al. (2015b), it is not clear which of them is responsible for the detected –ray emission.

Given that the spectral index of the –ray source, according to the 1FHL catalogue, is , its counterpart is more likely a flat spectrum radio quasar (FSRQ) than a BL Lac (Ackermann et al., 2015). We were not able to find any radio counterpart association in public surveys for the NLS1 potentially associated with 1FHL J1410.4+7408 A. Although NLS1 have been indicated as responsible for –ray as well as X–ray emission (e.g. Abdo et al., 2009b; Foschini et al., 2015, and references therein), the fact that it is not detected at radio bands brings up the possibility that this association is the product of a contamination of the sample due to the relative width of the Fermi positional error boxes. Only radio loud NLS1 have been detected in high energies.

Likewise, the BL Lac object probably associated with 1FHL J1410.4+7408 B also does not show radio emission. It is important to note that, if confirmed, the BL Lac object 1FHL J1410.4+7408 B would be one of the very few radio quiet –ray emitting BL Lac objects identified to date. Similar recent cases can be found in Paggi et al. (2014) and in Ricci et al. (2015).

To be conservative, it is thus safe to say that it is still not clear which of the two sources is the actual –ray emitter, or that the two objects are possibly contributing to the total –ray flux detected with Fermi. However, given the above considerations, it is more likely that the counterpart to this 1FHL –ray source is the BL Lac object associated with 1FHL J1410.4+7408 B.

Regarding the NLS1 object associated with 1FHL J1410.4+7408 A, a central black hole mass value can be estimated through measuring the FWHM and flux of the line (Kaspi et al., 2000; Wu et al., 2004) corrected for foreground galactic absorption. This allows us to infer a mass of for the black hole.

5.3 The case of 1FHL J1115.0-0701

We classified the optical counterpart of the X–ray source found within the 1FHL J1115.0-0701 positional uncertainty ellipse as a high–redshift quasar, with . This value, in turn, allows us to estimate a luminosity distance of Gpc, assuming , and . Following Park et al. (2013), we measured the flux and width of the CIV emission line together with the flux level of the continuum at 135 nm (rest–frame), both corrected for foreground galactic absorption, to obtain an estimate for the mass of its central black hole. This resulted in , which is within the range of expected black hole masses for this kind of AGN (Vestergaard & Peterson, 2006). Moreover, the above distance estimate implies an X–ray luminosity of in the 2–10 keV band, whereas the black hole mass corresponds to an Eddington luminosity value . Adopting a correction factor to obtain the X–ray bolometric luminosity (Ho, 2009), we find an Eddington ratio of . Assuming this quasar is the real counterpart for the 1FHL source, its –ray luminosity results in . This value, although rarely reached, is within the range expected for –ray emitting FSRQs (Cavaliere & D’Elia, 2002).

However, Petrov et al. (2013), Massaro et al. (2013a), and Schinzel et al. (2015) proposed a potential association of this Fermi source with a radio object (NVSS J111511–070238) located at a distance from the X–ray source found by Landi et al. (2015b). The radio source NVSS J111511–070238 is located at a distance of 2.5 arcmin from the 1FHL source, while the X–ray source lies at a distance of 3.2 arcmin from the latter. These two objects are not positionally consistent with each other. Therefore, this suggests that there may be two AGN within the Fermi error ellipse, a radio emitting one and an X–ray emitting one, which is the one we classify as a quasar.

In an attempt to discard one of the two proposed counterparts, we searched for archival multiwavelength data for both sources. We found no radio emission at the position of the X–ray quasar, suggesting that the object is possibly radio quiet and/or too cosmologically distant to be detected in the NVSS. However, this non–detection does not completely rule out the quasar as the real counterpart. Figure 14 of Abdo et al. (2009a) suggests a connection between radio luminosities and the –ray spectral indices obtained with the whole energy band at which Fermi/LAT works (i.e. 20 MeV to 300 GeV). If this object falls on the faint side of the connection (), shallow radio surveys are not able to detect any emission: indeed, at a redshift that luminosity would correspond to a flux density of , which is well below the detection threshold of the NVSS ().

Moreover, given that the spectral index across the whole Fermi/LAT energy range (, Acero et al., 2015) for this –ray source is an intermediate value between those of each kind, we cannot determine whether it is a BL Lac or a FSRQ.

On the other hand, its –ray spectral index above 10 GeV () is too low for typical FSRQs, but rather normal for BL Lac objects (Ackermann et al., 2013).

In conclusion, although no other high–energy emitting source was found within the 1FHL positional uncertainty ellipse, we cannot rule out the possibility that this quasar is a background object and that the potential association is actually spurious. To conclusively pinpoint the true association it is necessary to obtain a spectrum of the optical counterpart of the above mentioned radio source, which shows a magnitude of in the USNO-B1.0 catalogue.

6 Conclusions

We obtained optical spectra for 14 potential associations with –ray sources from the 1FHL catalogue, which were selected on the basis of their X–ray emission. These are our findings:

  1. From these spectra, it is clear that 12 of these objects correspond to blazars belonging to the BL Lac class, with non-thermal continua and no spectral features. There are two exceptions: U0750-02519189, associated with 1FHL J0639.6-1244, whose host galaxy’s spectroscopic signature is visible and allowed us to place it at a redshift of ; and U1530-0317394, associated with 1FHL J2002.6+6303, which presents absorption from an intervening medium, placing it at a minimum redshift . The other 10 BL Lacs remain without a value for their redshifts.

  2. At least 8 out of the 12 BL Lacs present spectral indices in agreement with a synchrotron peak at a frequency higher than , meaning they are likely candidates to be detected at TeV energies.

  3. The X–ray counterpart within the field of 1FHL J1115.0-0701 presents strong, broad optical emission lines at a redshift of , indicating that it is an AGN of the quasar class. By measuring the flux and width of the CIV emission line, we could estimate the mass of the central black hole as . Assuming this is the real counterpart for 1FHL J1115.0-0701, its luminosity would be and . However, from multiwavelength considerations, we cannot rule out the possibility that this quasar is a background object and that its potential association with the –ray source is the product of statistical contamination. Further analysis is needed, in particular concerning the other object proposed as the real counterpart, radio source NVSS J111511–070238.

  4. U1575–03416943, potentially associated with 1FHL J1410.4+7408 A, shows relatively narrow but strong emission lines at a redshift of . Given its optical spectral characteristics, we classified it as a NLS1. For this object we infer a central black hole mass of .

  5. Given that the source 1FHL J1410.4+7408 was potentially associated with objects A (a NLS1) and B (a BL Lac), we suggest -to be conservative- that it is still not clear which of the two sources is the actual –ray emitter, or if both of them are contributing to the total –ray emission. However, it is more likely the BL Lac object associated with 1FHL J1410.4+7408 B.

  6. Our optical spectroscopy confirmed all the counterpart candidates of the X–ray sources potentially associated with 1FHL objects selected for this paper, with 1FHL J1115.0–0701 as the only possible exception. We were able to classify all of them as extragalactic high–energy active nuclei. This strengthens the utility of the proposed approach - crossmatching –ray positions to soft X–ray ones, improving accuracy, then completing the identification process with optical follow–up work and multiwavelength archival data.

E. J. Marchesini would like to thank Francesco Massaro and Paola Grandi for the useful discussions on this work, and Gianluca Israel for coordinating the NOT observations and for useful comments. N. Masetti thanks the Facultad de Ciencias Astronómicas y Geofísicas de La Plata for the warm hospitality during the preparation of this paper. We thank Roberto Gualandi for night assistance at the Loiano telescope, and Gloria Andreuzzi for coordinating our service mode observation at the TNG. We also acknowledge the Italian Space Agency financial support (ASI/INAF agreement n. 2013-025.R.0). This work is funded under the co-tutoring agreement between University of Turin and University of La Plata.


  1. http://www.asdc.asi.it/
  2. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.


  1. Abdo, A. A., Ackermann, M., Ajello, M., et al. 2010, ApJ, 715, 429
  2. Abdo, A. A., Ackermann, M., Ajello, M., et al. 2009a, ApJ, 700, 597
  3. Abdo, A. A., Ackermann, M., Ajello, M., et al. 2009b, ApJ, 707, L142
  4. Acero, F., Ackermann, M., Ajello, M., et al. 2015, ApJS, 218, 23
  5. Ackermann, M., Ajello, M., Allafort, A., et al. 2013, ApJS, 209, 34
  6. Ackermann, M., Ajello, M., Atwood, W. B., et al. 2015, ApJ, 810, 14
  7. Ackermann, M., Ajello, M., Atwood, W. B., et al. 2016, ApJS, 222, 5
  8. Atwood, W. B., Abdo, A. A., Ackermann, M., et al. 2009, ApJ, 697, 1071
  9. Begelman, M. C., Blandford, R. D., & Rees, M. J. 1980, Nature, 287, 307
  10. Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245
  11. Cavaliere, A. & D’Elia, V. 2002, ApJ, 571, 226
  12. Condon, J. J., Cotton, W. D., Greisen, E. W., et al. 1998, AJ, 115, 1693
  13. Evans, P. A., Osborne, J. P., Beardmore, A. P., et al. 2014, ApJS, 210, 8
  14. Foschini, L., Berton, M., Caccianiga, A., et al. 2015, A&A, 575, A13
  15. Fossati, G., Maraschi, L., Celotti, A., Comastri, A., & Ghisellini, G. 1998, MNRAS, 299, 433
  16. Fukugita, M., Shimasaku, K., & Ichikawa, T. 1995, PASP, 107, 945
  17. Georganopoulos, M., Finke, J. D., & Reyes, L. C. 2010, ApJ, 714, L157
  18. Ghisellini, G., Tavecchio, F., Foschini, L., et al. 2010, MNRAS, 402, 497
  19. Goodrich, R. W. 1989, ApJ, 342, 224
  20. Ho, L. C. 2009, ApJ, 699, 626
  21. Kalberla, P. M. W., Burton, W. B., Hartmann, D., et al. 2005, A&A, 440, 775
  22. Kaspi, S., Smith, P. S., Netzer, H., et al. 2000, ApJ, 533, 631
  23. Landi, R., Bassani, L., Stephen, J. B., et al. 2015a, IASF Bologna Internal Report, 651
  24. Landi, R., Bassani, L., Stephen, J. B., et al. 2015b, A&A, 581, A57
  25. Landi, R., Bassani, L., Stephen, J. B., et al. 2015c, Proceedings of ”Swift: 10 Years of Discovery”
  26. Landoni, M., Massaro, F., Paggi, A., et al. 2015, AJ, 149, 163
  27. Mankuzhiyil, N., Persic, M., & Tavecchio, F. 2010, ApJ, 715, L16
  28. Masetti, N., Sbarufatti, B., Parisi, P., et al. 2013, A&A, 559, A58
  29. Massaro, E., Maselli, A., Leto, C., et al. 2015a, Ap&SS, 357, 75
  30. Massaro, F., D’Abrusco, R., Paggi, A., et al. 2013a, ApJS, 209, 10
  31. Massaro, F., Landoni, M., D’Abrusco, R., et al. 2015b, A&A, 575, A124
  32. Massaro, F., Paggi, A., Errando, M., et al. 2013b, ApJS, 207, 16
  33. Massaro, F., Tramacere, A., Cavaliere, A., Perri, M., & Giommi, P. 2008, A&A, 478, 395
  34. Monet, D. G. 1998, in Bulletin of the American Astronomical Society, Vol. 30, American Astronomical Society Meeting Abstracts, 1427
  35. Monet, D. G., Levine, S. E., Canzian, B., et al. 2003, AJ, 125, 984
  36. Mukai, K. 1993, Legacy, vol. 3, p.21-31, 3, 21
  37. Osterbrock, D. E. & Pogge, R. W. 1985, ApJ, 297, 166
  38. Padovani, P. & Giommi, P. 1995, ApJ, 444, 567
  39. Paggi, A., Milisavljevic, D., Masetti, N., et al. 2014, AJ, 147, 112
  40. Park, D., Woo, J.-H., Denney, K. D., & Shin, J. 2013, ApJ, 770, 87
  41. Petrov, L., Mahony, E. K., Edwards, P. G., et al. 2013, MNRAS, 432, 1294
  42. Ricci, F., Massaro, F., Landoni, M., et al. 2015, AJ, 149, 160
  43. Rieke, G. H. & Lebofsky, M. J. 1985, ApJ, 288, 618
  44. Schinzel, F. K., Petrov, L., Taylor, G. B., et al. 2015, ApJS, 217, 4
  45. Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
  46. Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163
  47. Stephen, J. B., Bassani, L., Landi, R., et al. 2010, MNRAS, 408, 422
  48. Vestergaard, M. & Peterson, B. M. 2006, ApJ, 641, 689
  49. Voges, W., Aschenbach, B., Boller, T., et al. 1999, A&A, 349, 389
  50. Wu, X.-B., Wang, R., Kong, M. Z., Liu, F. K., & Han, J. L. 2004, A&A, 424, 793
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description