text:
Home All issues Volume 625 (May 2019) A&A, 625 (2019) A26 Full HTML
Volume 625, May 2019
2. PKS 2251+11
3. Data reduction
4. Spectral analysis
5. Timing analysis
X-ray analysis of the accreting supermassive black hole in the radio galaxy PKS 2251+11
S. Ronchini1,2, F. Tombesi2,3,4,5, F. Vagnetti2, F. Panessa6 and G. Bruni6
1 Gran Sasso Science Institute (GSSI), Viale Francesco Crispi, 7, 67100 L'Aquila, AQ, Italy
e-mail: samuele.ronchini@gssi.it
2 Department of Physics, University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA
4 NASA/Goddard Space Flight Center, Code 662, Greenbelt, MD 20771, USA
5 INAF-Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monteporzio Catone, Italy
6 INAF-Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere 100, 00133 Roma, Italy
Context. We have investigated the dichotomy between jetted and non-jetted active galactic nuclei (AGNs), focusing on the fundamental differences of these two classes in the accretion physics onto the central supermassive black hole (SMBH). We tested the validity of the unification model of AGNs through the characterization of the mutual interaction between accreting and outflowing matter in radio galaxies.
Aims. Our aim is to study and constrain the structure, kinematics and physical state of the nuclear environment in the broad line radio galaxy (BLRG) PKS 2251+11. The high X-ray luminosity and the relative proximity make such AGN an ideal candidate for a detailed analysis of the accretion regions in radio galaxies. The investigation will help to shed light on the analogies and differences between the BLRGs and the larger class of radio-quiet Seyfert galaxies and hence on the processes that trigger the launch of a relativistic jet.
Methods. We performed a spectral and timing analysis of a ∼64 ks observation of PKS 2251+11 in the X-ray band with XMM-Newton. We modeled the spectrum considering an absorbed power law superimposed to a reflection component. We performed a time-resolved spectral analysis to search for variability of the X-ray flux and of the individual spectral components.
Results. We find that the power law has a photon index Γ = 1.8 ± 0.1, absorbed by an ionized partial covering medium with a column density NH = (10.1 ± 0.8) × 1023 cm−2, a ionization parameter log ξ = 1.3 ± 0.1 erg s−1 cm and a covering factor f ≃ 90%. Considering a density of the absorber typical of the broad line region (BLR), its distance from the central SMBH is of the order of r ∼ 0.1 pc. An Fe Kα emission line is found at 6.4 keV, whose intensity shows variability on timescales of hours. We derive that the reflecting material is located at a distance r ≳ 600rs, where rs is the Schwarzschild radius.
Conclusions. Concerning the X-ray properties, we found that PKS 2251+11 does not differ significantly from the non-jetted AGNs, confirming the validity of the unified model in describing the inner regions around the central SMBH, but the lack of information regarding the state of the very innermost disk and SMBH spin still leaves unconstrained the origin of the jet.
Key words: galaxies: active / galaxies: nuclei / accretion, accretion disks
© ESO 2019
Accretion onto supermassive black holes (SMBHs) is the physical mechanism powering active galactic nuclei (AGNs). As such, these sources are very efficient at converting the gravitational energy of the accreting mass in other forms of energy, as radiation or powerful outflows. The primary radiation emitted by the accreting material is reprocessed by the surrounding nuclear environment, so that the AGN is observable at all wavelengths, from radio to γ-rays. While there is consensus about what powers AGN, the structure of the nuclear environment is still a matter of debate. The unified model of AGNs (e.g. Antonucci 1993) posits that all active galaxies share a common structure, which can be summarized with a few fundamental components: i) a central SMBH; ii) an accretion disk; iii) a dusty obscuring torus, typically on the same plane of the accretion disk; and iv) outflows, in the form of highly collimated relativistic jets, or wide-angle nuclear winds (Padovani et al. 2017). According to the unified model, the distinction between unobscured (Type 1) and obscured (Type 2) AGNs is related to the inclination of the line of sight with respect to the plane of the accretion disk (Urry & Padovani 1995). Radio-loud quasars and less-luminous radio galaxies are capable of launching powerful, relativistic jets, while radio-quiet QSOs and Seyfert galaxies have jets that are much less powerful (the role of jet production in the AGN classification is reviewed by Padovani 2017). The mechanism responsible for the launching and the collimation of the relativistic jet is an open issue, and is likely related to the interaction between the magnetic field and the accretion disk (e.g. Romero et al. 2017, Keppens & Meliani 2010).
In this regard, X-ray observations provide a powerful tool for the investigation of the accretion-ejection physics in the neighborhood of the SMBH (e.g. Matt et al. 2007; Turner & Miller 2009; Reynolds 2016). While non-jetted AGNs are relatively well studied in the X-rays, we have a limited sample of radio galaxies whose X-ray properties are well constrained. For this reason we cannot yet confidently affirm that the underlying structure of the nuclear environment is the same for both non-jetted and jetted AGNs (e.g. Gliozzi et al. 2007). Since the fraction of absorbed AGN is comparable among non-radio galaxies and radio galaxies (Panessa et al. 2016), they could share a common obscuring structure, as predicted by the unified model. The presence or not of systematic differences in the X-ray properties between these two populations would help to clarify the role of the accretion processes in the triggering of the jet. AGNs show similarities with stellar BH binaries (Merloni et al. 2003), where the X-ray luminosity and the hardness of the X-ray spectrum are related with the production of jets and winds (Ponti et al. 2012; Fender & Muñoz-Darias 2016).
In this regard, the broad line radio galaxies (BLRGs) are especially suitable for high quality X-ray studies, given that they have the highest X-ray fluxes in the radio-loud population. The inclination angle between the line of sight (l.o.s.) and the perpendicular to the accretion disk in BLRGs has an intermediate value, meaning that the radiation coming out from the nuclear region is neither suppressed by the obscuring torus, nor overwhelmed by the relativistically boosted emission of the jet, as in blazars. Thanks to this characteristic, we are able to observe directly the optical emission of the broad line region (BLR) and we can also investigate the structure, the geometry, and the physics of the nuclear environment down to sub-pc scales.
Since the early observations with X-ray telescopes, radio loud (RL) AGNs appear slightly more luminous in the X-ray band, compared to the radio quiet (RQ) counterpart with comparable optical luminosity (Worrall et al. 1987; Chiaraluce et al. 2018). RL AGNs have also slightly flatter power law continuum, with ⟨ΓRL⟩ ∼ ⟨ΓRQ⟩ − 0.5 (e.g. Lawson & Turner 1997). However, these early results were affected by the low sensitivity of the instruments. For instance, Sambruna et al. (1999) found only a weak indication that the 2–10 keV spectra of BLRGs are flatter than those of Seyferts 1 galaxies. Wozniak et al. (1998) found in a sample of five BLRGs an average Fe Kα equivalent width (EW) of ∼100 eV and a Compton hump significantly weaker compared to those observed in RQ AGNs. The weakness of reflection components in BLRGs was confirmed by Eracleous et al. (2000), who proposed that this effect may be due to a small solid angle subtended by the disk to the primary continuum. This scenario is compatible with two-temperature disks, optically thick in the outer part and truncated in the inner part. The truncation may be induced by an advection-dominated accretion flow (ADAF) or ion-supported tori.
On the other hand, Ballantyne et al. (2002) suggest that the weakness of reflection features is not necessarily due to geometrical factors. Instead, they propose that the reprocessing by an ionized accretion disk could produce a similar effect, discarding the hypothesis that the RL–RQ dichotomy, and hence the production of the jet, is due to an intrinsic difference in the disk accretion state. In fact, other fundamental parameters could play a significant role in the production of the jet, such as high accretion rates and/or high values of mass and spin of the SMBH. Nonetheless, it is still not clear which combination of these parameters is the most favorable to trigger the jet emission (Chiaberge et al. 2015; Chiaberge & Marconi 2011). Ballantyne (2007) claims that the accretion geometry of RL AGNs could be related to the accretion efficiency, in turn linked to the AGN luminosity. In particular, for bolometric luminosities Lbol < 0.01LEdd the accretion transits to ADAFs, explaining the absence of reflection by the inner part of the disk (LEdd is the Eddington luminosity). For Lbol > 0.01LEdd, the disk is not truncated and the reflection can extend down to the innermost stable circular orbit (ISCO). The presence of reflecting material close to the SMBH is responsible for the emission of a relativistically broadened Fe Kα line, whose evidence is mixed in the case of BLRGs. The Fe Kα line can be originated by several components, such as the accretion disk, the BLR, or the inner part of the obscuring torus. In BLRGs each component can contribute differently, producing a final Fe Kα line width that varies case by case (e.g. Tombesi et al. 2010a; Ogle et al. 2005; Lohfink et al. 2013; Sambruna et al. 2009; Lohfink et al. 2015).
In the discussion of Sambruna et al. (2009), the authors infer that there is also a dichotomy in the outflow typology between BLRGs and Seyfert galaxies. In this scenario, accretion disk winds would be produced only by Seyferts, while the jet is a prerogative of radio galaxies. If we suppose that the bulk of accretion energy is used for winds acceleration, the jet formation is prevented, thus explaining the lack of jets in Seyferts. Nevertheless, the subsequent work of Tombesi et al. (2014) controverts this scenario, demonstrating that the production of mildly-relativistic disk winds is not a prerogative of RQ AGNs. In fact ultra fast outflows (UFOs) are found in both RQ and BLRGs (Tombesi et al. 2010b, 2014; Gofford et al. 2013; Reeves et al. 2010; Longinotti et al. 2015), indicating that their origin is somewhat independent of the formation of the relativistic jet. On the other hand, the presence of this latter remains a prerogative of RL galaxies.
Recent X-ray observations with XMM-Newton, Suzaku and NuSTAR (Sambruna et al. 2011; Ballantyne et al. 2014; Reynolds et al. 2015; Ursini et al. 2018) suggest that the accretion structure in BLRGs and in Seyfert galaxies is similar, therefore indicating that the separation in different classes is subtle. Instead, on the basis of these last results, the first ones can be considered as a sub-class of the second ones.
PKS 2251+11 is a BLRG with a redshift z = 0.3255, derived from optical emission lines. Mor et al. (2009), modeling the infrared spectrum emitted by the dusty torus, derived the angle i between the direction of the jet and the l.o.s., obtaining i = 67°. This result indicates that PKS 2251+11 may be at the border between Type 1s and Type 2s, possibly intercepting part of the obscuring torus. Since the authors do not indicate the uncertainty associated with the estimation of i, in our analysis we will assume an inclination angle contained in the range 50° < i < 70°. Besides, the authors estimated an opening angle of the torus equal to σ = 15°, whose value is one of the smallest among the other sources in the sample.
Wandel (1991) used two independent methods for estimating the mass of the central SMBH MBH in this object, obtaining MBH ≃ 1.4 × 109 M⊙ and MBH ≃ 1.7 × 109 M⊙, with a fractional difference of ∼17%. In the same article the authors also derived log [ηṀc2/LEdd] = −1.52 and Ṁ ≃ 1 M⊙ yr−1 (Ṁ is the mass accretion rate and η is the accretion efficiency).
Davis & Laor (2011), using a dynamical approach, estimated MBH ≃ 7.2 × 108 M⊙. Assuming the optical emission dominated by the accretion disk, the authors derive also a mass accretion rate of Ṁ = 4.6 M⊙ yr−1, which is not far from the value obtained by Wandel (1991). Other derived quantities are Lbol = (1.35 ± 0.03) × 1046 erg s−1 and an accretion efficiency η = 0.066. Vestergaard (2002), through single-epoch spectroscopic measurements, obtained , comparable both with the estimates given by Davis & Laor (2011) and Wandel (1991). In the following we will consider only the value given by Vestergaard (2002), as it is likely the most accurate estimate.
Laor & Behar (2008), studying the correlation between the radio and X-ray luminosities in a sample of both RL and RQ AGNs, report for PKS 2251+11 these quantities: LR = νLν|ν=6 cm = 1.15 × 1043 erg s−1, where LR is the total radio luminosity at 6 cm (taken from Kellermann et al. 1989, which also found that the contribution of the core to the radio luminosity is less than 1%); LX = 1.15 × 1044 erg s−1, with LX is the X-ray luminosity in the energy range E = 0.2−20 keV; αox = 0.372 log [Fν = 2 keV/Fν = 3000 Å] = −1.86; log R = 2.56, where R is the radio loudness, equivalent to R = 1.36 × 105L5/LB, with L5 = Lν|ν = 5 GHz and LB = Lν|ν = 4400 Å. Sambruna et al. (1999), performing an X-ray spectral analysis of RL AGNs observed with ASCA, reported radio archival data of PKS 2251+11. They derived the parameter logℛ = [radiocorepower/lobesradiopower] = −1.51, which indicates that the core contributes only to 3% of the total radio luminosity. In the same article the X-ray spectrum of PKS 2251+11 is analyzed and the adopted model is an absorbed power law. The derived best fit parameters are and . Especially for E < 2 keV, absorption and emission features appear rather complex. The authors tried to add a Gaussian line in correspondence of the Fe Kα line, keeping fixed during the fit the energy at 6.4 keV and the width at σga = 50 eV. They derive an upper limit of the equivalent width of EW < 315 eV.
PKS 2251+11 was observed with XMM-Newton on 2011 December 18, for a total exposure of 63.8 ks. In this work we consider the EPIC-pn data. The detector operated in full window imaging mode. Data reduction and analysis were performed following the SAS standard procedure1. In order to check the presence of particle flaring background, we considered the entire field of view and we selected only the photons with energy in the range E = 10−12 keV. Then we plotted a light curve of the selected photons, excluding from the initial observation all the intervals of time in which the count rate is higher than 0.6. Subsequently, we extracted a circular region centered on the source, with a radius of 35″. The background region is of the same shape and dimension but centered in an area free of emission from point sources, located in the same CCD. The test for the presence of pile-up gave a negative response. After the filtering procedure, the net exposure of the observation was reduced to 57.3 ks. Along with the cleaned spectrum, a redistribution matrix file (RMF) and an ancillary response function (ARF) were created with standard SAS tools. The spectral data were grouped choosing a minimal threshold of 25 photons per bin and a χ2 statistic is adopted. Only in the case of time resolved spectroscopy (see below) the minimal threshold is lowered to five or ten photons per bin and a C-statistic is adopted. Unless otherwise specified, the errors are reported with at 1σ level of confidence, while the upper and lower limits are reported with a 90% level of confidence.
Our analysis is performed using the Heasarc v. 6.21 and XSPEC v. 12.9.1. We began trying to fit the data with an absorbed power law, following the standard assumption that a hot corona comptonizes the soft seed photons emitted by the accretion disk (e.g. Haardt & Maraschi 1991).
4.1. Neutral total covering absorber
First we included only the absorption due to the interstellar medium (ISM) in our Galaxy, for which Dickey & Lockman (1990) estimate a column density . For the estimate of the absorption cross section, we refer to the Tuebingen-Boulder model (Wilms et al. 2000), which in XSPEC is indicated as tbabs. The fit gives a χ2/d.o.f. = 917.5/369. Therefore the Galactic absorption is not sufficient to fit the spectrum and we added an absorption component due to neutral gas in the AGN host galaxy, but this does not improve the fit (χ2/d.o.f. = 917.5/368).
4.2. Neutral partial covering absorber
Then we tested the hypothesis of a neutral partial covering absorption, modeled in XSPEC as pcfabs. The resulting model is written in XSPEC language as zpcfabs*tbabs*zpo. Adding just one parameter, the fit improves to a value χ2/d.o.f. = 448.3/367. The validity of this improvement is also confirmed by the ftest, which gives a confidence larger than 5σ. The derived best fit parameters are , f = 0.85 ± 0.01 and Γ = 1.76 ± 0.04, where NH is the column density of the gas in the source host galaxy, f is the covering factor, in other words, the fraction of the solid angle subtended by the absorbing medium, and Γ the photon index of the power law. The comparison between this model and the EPIC-pn spectrum is showed in Fig. 1.
Comparison between the EPIC-pn spectrum and the model zpcfabs*tbabs*zpo. The data to model ratio is showed in the bottom panel.
4.3. The Fe Kα line
As can be seen in Fig. 2, there is an excess of counts between 6 and 7 keV, which we identify with the Fe Kα fluorescence line. This last is modeled with a Gaussian profile, with a centroid Ega and a width σga. The model is written as zpcfabs*tbabs*(zpo+zga). Letting both the parameters Ega and σga vary freely during the fit, we find that the line is unresolved, since we obtain only an upper limit for σga ≤ 120 eV. The inclusion of this component improves the fit to χ2/d.o.f. = 424.8/364. The best fit value for the energy is Ega = 6.41 ± 0.03 keV. The significance for the addition of this line is > 3.7σ. In the following, since the line is unresolved, we fixed the width σga at 10 eV.
Zoom of the data to model ratio in the Fe K band at energies E = 6−7 keV for zpcfabs model. The bump around 6.4 keV suggests a possible neutral Fe Kα emission line.
4.4. Ionized partial covering absorber
A further improvement of the fit occurs if we relax the hypothesis of neutral absorbing gas, which is no more valid if the primary continuum is particularly intense and/or if the absorber is located close to the X-ray source. In this case we substituted in XSPEC the model pcfabs with the model zxipcf (Reeves et al. 2008), which introduces the ionization parameter ξ = Lion/(nr2), where Lion is ionizing luminosity in the energy range E = 13.6 eV–13.6 keV, while n and r are the density and the distance form the SMHB of the absorber, respectively. The fit gives a high improvement to χ2/d.o.f. = 382.9/364. The best fit values are , , f = 0.88 ± 0.01 and Γ = 1.78 ± 0.05. The comparison between this model and the spectrum is showed in Fig. 3. Until now we have assumed that the redshift z of the source and that of the absorber zabs are the same, namely that this last is at rest in the source reference frame. Then, if we let free zabs during the fit, we can explore the possibility that the absorber has a motion along the line of sight in the rest frame of the source. However, given the low energy resolution of the EPIC-pn and relatively low soft X-ray flux of the source, we are not able to statistically constrain the kinematics of the absorber.
Comparison between the EPIC-pn spectrum and the model zxipcf*tbabs*(zpo+zga). With respect to the Fig. 1 the agreement improves especially in the band E = 0.5−1 keV, where the presence of ionization lines and edges most influences the overall shape of the spectrum. The data to model ratio is showed in the bottom panel.
From the final best-fit model including zxipcf we derive an absorbed flux in the energy range E = 0.5−10 keV equal to . The unabsorbed flux is , which is the flux emitted by the primary continuum without considering the the suppression due to absorption. The corresponding intrinsic X-ray luminosity in the energy range E = 0.5−10 keV is . Therefore the absorption causes a significant decrease of the intrinsic flux equal to [Funabs − Fabs]/Funabs ≃ 47%.
4.5. The pexmon model
Finally we tried to investigate the nature of the Fe Kα emission line using the reflection model pexmon (Nandra et al. 2007) which introduces the parameter R = Ω/2π, namely the fraction of the solid angle covered by the reflecting medium, seen by the primary X-ray source. We assume a solar abundance, a high-energy cutoff at 150 keV, an inclination angle i = 60° (in the middle of our confidence range 50° < i < 70°), while we let free Γ, R and the parameters of the absorber. We derive , , f = 0.87 ± 0.01, Γ = 1.79 ± 0.05 and . Even assuming an inclination angle in the range between 50° and 70°, the reflection factor does not change significantly, being in any case compatible with 1. The results from zxipcf and pexmon models are summarized in Table 1.
Values of the best-fit model including a Gaussian emission line for the Fe Kα or pexmon.
5.1. X-ray variability
In order to check for X-ray variability, we created a light curve of the count rate in the energy band E = 0.3−10 keV. For different bin times (100 s, 500 s, 1000 s, 5000 s and 10 000 s) we have calculated: i) the average value ⟨C⟩ of the count rate; ii) the χ2 probability p, which indicates the probability that the observed variability is due to chance. As a threshold, we consider significant the variability only when 1 − p > 99.7% (3σ level of confidence); iii) the , with Cmax and Cmin the highest and lowest points in the light curve, while σmax and σmin the respective errors of Cmax and Cmin; iv) the normalized excess variance , where S2 is the variance of the light curve, that is , where the sum is extended over all the N points and ⟨C⟩ is the average value of the count rate; ⟨σ2⟩ is the average value of the errors associated to each point.
For a bin time of 500 s we report the light curve of the count rate in Fig. 4. From Table 2 we can see that the variability is not significant for any choice of bin time.
Light curve of the photon count rate in the energy range E = 0.3−10 keV, from the EPIC-pn observation. The horizontal blue line indicates the average value of the count rate. A, B, and C indicate the time intervals defined in Sect. 5.2.
Variability estimator values for different choices of bin time.
5.2. Time resolved spectral analysis
At this point, we tested the variability of the individual spectral components through a time resolved spectral analysis. First, we have produced two light curves, one in the soft X-ray band E = 0.5−2 keV and the other in the hard X-ray band E = 5−10 keV (the energies are referred to the source reference frame). Then we computed the hardness ratio as HR(t) = C5−10 keV(t)/C0.5−2 keV(t), where C5−10 keV(t) and C0.5−2 keV(t) are the hard and soft light curves, respectively. From the Fig. 5, the HR is almost constant apart in some time intervals where it increases during a time scale of 104 s. We divided the whole exposure in three sub-intervals, namely the interval A → [0 ks < t < 10 ks]+[16 ks < t < 52 ks]+[56 ks < t < 62 ks]; the interval B → 10 ks < t < 16 ks; the interval C → 52 ks < t < 56 ks. For each of these intervals we have extracted the spectrum. Since the intervals B and C have a very short exposure, the collected photons are ∼1/10 of those of the total observation, with subsequent poor statistic for spectral parameters determination. So we first tried to merge B and C, gaining in S/N, but loosing information on the individual intervals. The new interval BC has [10 ks < t < 16 ks] + [52 ks < t < 56 ks]. We analyzed at the same time the spectra from A and BC, with the model zxipcf*tbabs*(zpo+zga). Apart from , σga and the redshift of the components, all the other parameters are left free during the fit. No parameter changes significantly from A to BC, apart for the normalization of the Fe Kα line, which increases in BC, when the hardness ratio is higher.
Hardness ratio HR as a function of time, for a bin time choice of 2000 s. The horizontal solid line is the average value of HR. Around 16 ks and 55 ks the HR differentiates from its average value. A, B, and C indicate the time intervals defined in Sect. 5.2.
Then we analyzed A, B, and C separately. Since the counts in B and C are few, if we let the spectral parameters for A, B, and C vary freely, the fit does not converge, or the errors are large. So we assumed that, apart the normalization of the Fe Kα, all the parameters do not change during the observation, obtaining , where the superscript refers to the line normalization in A, B and C, respectively.
Apparently, within the errors, in A, B, and C the Nga is compatible with a constant. Although, since the exposure of C is too short, we cannot have a precise constraint on Nga, while the variability from A to B is more remarkable. In order to test the variability of Nga between A and B, we considered the contour plot of and in Fig. 6, where we drew the line . The green region shows the area in the parameter space where with a 90% level of confidence. As evident, it is considerably more probable that . As a further check, we tried to use the model zxipcf*tbabs*pexmon, following the same procedure described above, fixing all the parameters equal for A, B and C and letting free only the reflection parameter R. In A, B and C the reflection parameter assumes the values , and , respectively. They are all compatible within the errors, but looking at the contour plot of RA and RB we notice that the intersection between the 90% area and the region where RA > RB is extremely small. Therefore we can affirm that also the reflection parameter varies sensibly from A to B. Such result is in agreement with the increasing of Nga in the interval B. In fact, the greater is the solid angle covered by the reflector, the higher is the intensity of the reflection component. Finally we tried to vary the inclination angle i between 50° and 70°, always finding that RB ∼ 2 × RA, while RC ∼ RA.
Confidence contours for and . The straight black line is drawn in correspondence of . The green area is the intersection between the half-plane below the black line and the region contained inside the 90% contour.
In our spectral analysis of the X-ray spectrum of PKS 2251+11, the best-fit is obtained considering an absorbed power law, where the absorbing medium is ionized and partially covers the primary X-ray source. We also detect the presence of an unresolved Fe Kα emission line at 6.4 keV.
6.1. Location of the absorber
The ionization parameter , used in the photoionization models, contains information about the physical state of the absorber, which is likely to be stratified along the line of sight. The stratification implies that the gas has a value of ξ that changes with r. In this case r and n are defined as the inner radius of the absorber and the corresponding density, respectively. Usually the ionizing luminosity is well constrained by the spectral analysis, while the highest uncertainty is associated with r and n. An upper limit for r can be obtained writing NH ≃ nΔr, with Δr as the thickness of the absorber along the line of sight. Then, assuming that Δr < r we can write .
From the spectral analysis we see that the assumption of a single partial covering ionized medium is sufficient to give a good agreement with data. Therefore we can exclude that the absorption is due to a medium with a large range of ionization parameter and/or distributed along a broad range of distances from the center. If this were the case, the fit with a single absorbing component would not give the agreement that we obtain. Consequently, we can assume, as a first order approximation, that the absorber is composed by a single medium, whose thickness is much smaller than its distance from the center, namely Δr ≪ r, and whose ionization parameter is contained in a small range ξ0 − Δξ < ξ < ξ0 + Δξ, with Δξ ≪ ξ0. In this case we can write
In order to estimate Lion, we assumed that the ionizing continuum between 13.6 eV and 13.6 keV follows a power law, with the same photon index found in the X-ray band. In XSPEC we used the task clumin to obtain
which gives
Alternatively, we can also parametrize Δr = αr, with α an unknown constant. The photoionization model that we considered in our spectral analysis assumes a thin shell of absorbing material and therefore we can assume α ≪ 1. Thus we can write
and hence, for NH = 10.1 × 1022 cm−2 and log ξ = 1.33 erg s−1 cm
For comparison, we can consider the location of the BLR, which can be deduced using the HβFWHM = 4160 km s−1 = vBLR (Vestergaard 2002). Assuming a Keplerian orbit around the SMBH, we have
Therefore, for α ∼ 10−3 the ionized partial covering absorber can be identified with the BLR, while for 10−3 ≲ α ≪ 1 the absorber is more likely identified with the obscuring torus. Furthermore, we can use the definition of the ionization parameter ξ to write the distance r as a function of the density n of the absorber, obtaining:
If we consider a density n = 109 cm−3, typical of the BLR clouds (e.g. Snedden & Gaskell 1999), and using Lion = 1.24 × 1045 erg s−1, the distance of the absorber is r ∼ 0.1 pc. We notice that this distance is comparable with the previous estimate of the location of the BLR.
Confidence contours for RA and RB. The straight black line is drawn in correspondence of RA = RB. The green area is the intersection between the half-plane below the black line and the region contained inside the 90% contour.
6.2. Covering factor and filling factor of the absorber
Adopting the zxipcf model, we obtained a covering factor f = 0.88, meaning that the absorber is not homogeneous, but rather has a clumpy structure. In the following, we show how we can relate the covering factor f with the filling factor ℱ. Assuming that the absorber is composed by several distinct clouds, we can define N0 the number of clouds per unit volume and V̄ the average volume of a single cloud. Thus we can write
The covering factor, instead, is defined as
with ΔΩ the solid angle subtended by the primary X-ray source, while ΔΩabs is the portion of this solid angle covered by the absorber. If we call the typical dimension of a single cloud, then and we can distinguish two cases: 1) the thickness of the absorber and 2) . In the first case, since the linear dimension of the clouds is of the same order of magnitude of the thickness of the absorber, we can assume that the clouds do not overlap along the l.o.s. Thus the filling factor can be rewritten as
We find an interesting consequence: given a thin absorbing shell with a certain covering factor, we have ℱ ∼ f, independently on the distance from the primary source. This reasoning is no more valid for a thick shell, namely when . We can consider, for instance, a thin shell with a certain filling factor ℱ = N0V̄ ∼ f. Then, if we imagine a thick shell with the same value of ℱ, several clouds would overlap along the l.o.s. and a greater fraction of ΔΩ would be covered, implying ℱ < f. Thus we can conclude that, even if or , the covering factor f represents always an upper limit for the filling factor ℱ. In our case we have
We note that, even if in the thin shell limit we could assume ℱ ∼ f, N0 and V̄ would still remain degenerate.
6.3. Location and geometry of the reflector
Furthermore, analyzing the Fe Kα line, we can infer useful information about the location of the reflecting material. Firstly, we note that the best fit value of the line centroid is 6.41 keV, which already indicates qualitatively that the bulk of the reflector is lowly ionized. In order to quantify the level of ionization we refer to Matt et al. (1993), who studied the physical properties of an accretion disk illuminated by an ionizing continuum. In particular, in Fig. 1 of Matt et al. (1993) the centroid of the Fe Kα line is plotted as a function of the ionization parameter ξ. Combining this figure and the results of our spectral analysis, we can affirm that, at 90% level of confidence, Ega < 6.5 keV, which implies ξ < 400 erg s−1 cm. Thus, calling ξR, nR and rR the ionization parameter, the density and the distance of the reflector, respectively, we can write:
Analogously we can define ξA, nA and rA the ionization parameter, the density and the distance of the absorber, respectively. In general, the reflector and the absorber do not receive the same ionizing luminosity, due to the complexity of the nuclear geometry. In particular, if the reflector is much farther from the SMBH compared to the absorber, there is a time lag in the propagation of the ionizing continuum. Therefore we can parametrize , where the subscript "A" refers to the absorber, while "R" to the reflector. Using Eq. (7), we can write
which can be rewritten using the Eq. (3) as
Such relation imposes a lower limit for the location of the reflector, but it contains unknowns that cannot be directly derived from our analysis, such as λ, nA and nR. We can qualitatively deduce that the density of the reflector is likely much higher than that of the absorber, since the reflection component is not strong and the reflecting gas is less ionized than the absorbing gas. Nevertheless, this is not sufficient to derive a numerical constraint for a lower limit of rR.
Another interesting information about the location of the reflector comes from the width of the Fe Kα line, which appears not resolved. Indeed, if we let free the parameters Ega and σga during the fit, we find σga < 120 eV. This result is in accordance with what has been found in the literature for other BLRGs, which rarely show a relativistic broadened iron line. If we suppose that the broadening is due mostly to a Doppler kinematic effect, we can infer another constraint on the location of the reflector. Let us suppose that the reflector follows almost circular Keplerian orbits. In this configuration, part of the reflector moves toward the observer, part moves away, causing the Doppler broadening of the line. Since the orbital velocity increases at lower distances, we may say that an upper limit of σga implies a lower limit rin for the distance of the reflector. In order to find rin, we make the rough approximation
where σmax = 120 eV, Δv// = Δvsini and Δv = 2 vorb|rin. Therefore
For 50° < i < 70°, we have that 0.024 < β < 0.030. Then, knowing that
with , we obtain
where 600 rs ≲ rin ≲ 900 rs. Although, we stress that this lower limit for rR is related to the reflecting material that produces the observed narrow Fe Kα line. In principle, a fainter and broader iron line can be present in the spectrum, but not detectable with the S/N of our data. It could be also possible that the inner part of the disk (rR ≲ 600rs) does not contribute considerably to the emission of Fe fluorescence because its level of ionization is too high and most of the outer electrons are ripped off the atoms.
The pexmon model does not modify sensibly the best fit values of NH, log ξ, f and Γ. The reflection parameter R is constrained in the range 0.64 < R < 1.85, having assumed an inclination angle in the range 50° < i < 70°. Such result is compatible with a scenario where the reflector covers most of the solid angle illuminated by the primary source. If also the dusty torus contributes to the reflection, a value of R ∼ 1 implies that the torus has a flattened geometry, meaning that almost all the radiation emitted by the primary source is reflected toward the observer. The scenario of a flattened torus is also supported by Mor et al. (2009), who found an opening angle of only 15°. Anyway, the data quality is not good enough to infer further information about the geometry of the reflector.
6.4. Variability of the reflection component
The timing analysis of the source light curve does not show any significant evidence of variability of the total flux during the entire exposure. Then we investigated the variability of the hardness ratio. Two intervals, that we called B and C, of the duration of 6 ks and 4 ks respectively, show an HR significantly higher than the average value. We analyzed the spectrum in these intervals, in order to test the variability of the individual spectral components.
Neither the fit parameters associated with the absorber nor the properties of the power law change significantly when the HR is higher. Instead, the reflection component shows evidence of variability, especially in the interval B. If the Fe Kα line is modeled with a Gaussian, its normalization increases at least of a factor of two in B. As a consistency check, also using the pexmon model the reflection factor has an average value of ⟨R⟩ ≲ 1 in A, while R > 1 in B.
In order to explain the variability of the reflection component, we notice that the intensity of this last is directly proportional to the incoming primary flux. In the case of the Fe Kα line, since the fluorescence is due to the absorption of X-ray photons with E ≥ 7 keV, a variability of the incoming flux above 7 keV (F>7 keV) causes the variability of the line intensity. Therefore, we propose two different scenarios: i) We interpret the reflection variability as an effect of Compton thick clouds rapidly moving in the immediate vicinity of the X-ray primary source. If such clouds intercept the flux directed to the reflector, the flux F>7 keV is partly suppressed, otherwise it increases. In such scenario the variability timescales of the reflection component are related to the dynamical time scales of the obscuring clouds. Alternatively we could suppose that the obscuring clouds are not located between the primary source and the reflector, but rather between the reflector and the observer. Though, in this case, two drawbacks arise. First, if the obscuring clouds are on the line of sight, we should observe at the same time a variability of both the reflection component and the column density NH, which is not our case. Second, since we have derived a lower limit for the distance of the material that produces the Fe Kα line, the dynamical time scales of the obscuring clouds would be too long to explain the variability of the reflection on time scales of ∼104 s. ii) The reflection variability is directly caused by an intrinsic variability of the primary source luminosity, but since the narrow Fe Kα line is produced at a distance RR ≳ 600 rs, there is a net time lag between the arrival time of the primary continuum and the reflected component. The time lag would be at least of 60 days, which could explain why in a single exposure of ∼17 h, we do not observe an increase of the primary flux followed by the increase of the reflection component.
Through the X-ray analysis of an observation performed with the XMM-Newton observatory, we have obtained novel information about the geometry, kinematics, and physical state of the regions surrounding the accreting SMBH at the center of the BLRG PKS 2251+11. The X-ray spectrum is consistent with a primary component described by a power law, which is absorbed by an ionized partial covering medium. Considering a density of the absorber typical of the BLR, its distance from the SMBH is of the order of R = 0.1 pc. This estimate is comparable with the location of the BLR, estimated through the virial theorem and knowing the FWHM of the Hβ. Alternatively, if we assume lower values of density, it is not excluded that the absorber is located farther from the SMBH, in the zone of the dusty torus. The absorber is likely clumpy, in other words, composed by distinct clouds with a covering factor f ≃ 90% and a filling factor ℱ ≲ f. The spectral analysis confirms the presence of an unresolved Fe Kα line and the bulk of the emission occurs at a distance rR > 600rs.
Besides the intensity of the Fe Kα line, no other spectral parameters show significant variability during the observation. Due to the considerable distance between the reflector and the SMBH, the variability of the Fe Kα intensity is likely due to past variations of the primary flux. Nonetheless, a rearrangement of the absorber geometry may also be a valid alternative.
An interesting follow up investigation could be an observation with the NuSTAR observatory of the high-energy part (E > 10 keV) of X-ray spectrum. With such analysis we could see if the power law has the same photon index also at higher energies, understanding in this way whether other components, such as the radio jet, can contribute to the X-ray emission of this AGN. Furthermore the energy of the power law cut-off (typically around 100 keV) is directly connected with the temperature of the electrons of the hot corona.
It would be also interesting to extend this work to a multi-epoch X-ray observation of PKS 2251+11, exploring the variability on timescales of days or months. For instance the scenario of a delayed response of the reflection component after a variation of the primary flux could be further tested. The light curves of the primary continuum and the reflection component could be cross-correlated, similarly to the method adopted in reverberation mapping of the BLR in the optical/UV band. Possible evidence of delay could further constrain the location of the reflector. With an X-ray multi-epoch study we could also test the way in which the geometry of the absorber influences the variability of the spectrum at energies E < 2 keV.
Described by the threads on the web page https://www.cosmos.esa.int/web/xmm-newton/sas-threads
S. Ronchini, who carried out this work during his master thesis at the University of Rome "Tor Vergata", thanks the other authors for the valuable support. F. Tombesi acknowledges support by the Programma per Giovani Ricercatori - anno 2014 "Rita Levi Montalcini". G.Bruni acknowledges financial support under the INTEGRAL ASI-INAF agreement 2013-025. R01. The authors thank the anonymous referee for the constructive comments.
Antonucci, R. 1993, Annu. Rev. Astron. Astrophys., 31, 473 [Google Scholar]
Ballantyne, D. R. 2007, Mod. Phys. Lett. A, 22, 2397 [NASA ADS] [CrossRef] [Google Scholar]
Ballantyne, D. R., Ross, R. R., & Fabian, A. C. 2002, MNRAS, 332, L45 [NASA ADS] [CrossRef] [Google Scholar]
Ballantyne, D. R., Bollenbacher, J. M., Brenneman, L. W., et al. 2014, ApJ, 794, 62 [NASA ADS] [CrossRef] [Google Scholar]
Chiaberge, M., & Marconi, A. 2011, MNRAS, 416, 917 [NASA ADS] [CrossRef] [Google Scholar]
Chiaberge, M., Gilli, R., Lotz, J. M., & Norman, C. 2015, ApJ, 806, 147 [NASA ADS] [CrossRef] [Google Scholar]
Chiaraluce, E., Vagnetti, F., Tombesi, F., & Paolillo, M. 2018, A&A, 619, A95 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Davis, S. W., & Laor, A. 2011, ApJ, 728, 98 [CrossRef] [Google Scholar]
Dickey, J. M., & Lockman, F. J. 1990, Annu. Rev. Astron. Astrophys., 28, 215 [Google Scholar]
Eracleous, M., Sambruna, R., & Mushotzky, R. F. 2000, ApJ, 537, 654 [NASA ADS] [CrossRef] [Google Scholar]
Fender, R., & Muñoz-Darias, T. 2016, in The Balance of Power: Accretion and Feedback in Stellar Mass Black Holes, eds. F. Haardt, V. Gorini, U. Moschella, A. Treves, & M. Colpi, 65 [Google Scholar]
Gliozzi, M., Sambruna, R. M., Eracleous, M., & Yaqoob, T. 2007, ApJ, 664, 88 [NASA ADS] [CrossRef] [Google Scholar]
Gofford, J., Reeves, J. N., Tombesi, F., et al. 2013, MNRAS, 430, 60 [Google Scholar]
Haardt, F., & Maraschi, L. 1991, ApJ, 380, L51 [NASA ADS] [CrossRef] [Google Scholar]
Kellermann, K. I., Sramek, R., Schmidt, M., Shaffer, D. B., & Green, R. 1989, AJ, 98, 1195 [NASA ADS] [CrossRef] [Google Scholar]
Keppens, R., & Meliani, Z. 2010, in Numerical Modeling of Space Plasma Flows, Astronum-2009, eds. N. V. Pogorelov, E. Audit, & G. P. Zank, ASP Conf. Ser., 429, 91 [NASA ADS] [Google Scholar]
Laor, A., & Behar, E. 2008, MNRAS, 390, 847 [NASA ADS] [CrossRef] [Google Scholar]
Lawson, A. J., & Turner, M. J. L. 1997, MNRAS, 288, 920 [NASA ADS] [CrossRef] [Google Scholar]
Lohfink, A. M., Reynolds, C. S., Jorstad, S. G., et al. 2013, ApJ, 772, 83 [NASA ADS] [CrossRef] [Google Scholar]
Lohfink, A. M., Ogle, P., Tombesi, F., et al. 2015, ApJ, 814, 24 [NASA ADS] [CrossRef] [Google Scholar]
Longinotti, A. L., Krongold, Y., Guainazzi, M., et al. 2015, ApJ, 813, L39 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Matt, G. 2007, in The Central Engine of Active Galactic Nuclei, eds. L. C. Ho, & J. W. Wang, ASP Conf. Ser., 373, 125 [NASA ADS] [Google Scholar]
Matt, G., Fabian, A. C., & Ross, R. R. 1993, MNRAS, 262, 179 [NASA ADS] [CrossRef] [Google Scholar]
Merloni, A., Heinz, S., & di Matteo, T. 2003, MNRAS, 345, 1057 [NASA ADS] [CrossRef] [Google Scholar]
Mor, R., Netzer, H., & Elitzur, M. 2009, ApJ, 705, 298 [NASA ADS] [CrossRef] [Google Scholar]
Nandra, K., O'Neill, P. M., George, I. M., & Reeves, J. N. 2007, MNRAS, 382, 194 [NASA ADS] [CrossRef] [Google Scholar]
Ogle, P. M., Davis, S. W., Antonucci, R. R. J., et al. 2005, in X-Ray and Radio Connections, eds. L. O. Sjouwerman, & K. K. Dyer, 7.20 [Google Scholar]
Padovani, P. 2017, Nat. Astron., 1, 0194 [NASA ADS] [CrossRef] [Google Scholar]
Padovani, P., Alexander, D. M., Assef, R. J., et al. 2017, A&ARv, 25, 2 [Google Scholar]
Panessa, F., Bassani, L., Landi, R., et al. 2016, MNRAS, 461, 3153 [NASA ADS] [CrossRef] [Google Scholar]
Ponti, G., Fender, R. P., Begelman, M. C., et al. 2012, MNRAS, 422, L11 [NASA ADS] [CrossRef] [Google Scholar]
Reeves, J., Done, C., Pounds, K., et al. 2008, MNRAS, 385, L108 [NASA ADS] [CrossRef] [Google Scholar]
Reeves, J. N., Gofford, J., Braito, V., & Sambruna, R. 2010, ApJ, 725, 803 [NASA ADS] [CrossRef] [Google Scholar]
Reynolds, C. S. 2016, Astron. Nachr., 337, 404 [NASA ADS] [CrossRef] [Google Scholar]
Reynolds, C. S., Lohfink, A. M., Ogle, P. M., et al. 2015, ApJ, 808, 154 [NASA ADS] [CrossRef] [Google Scholar]
Romero, G. E., Boettcher, M., Markoff, S., & Tavecchio, F. 2017, Space Sci. Rev., 207, 5 [NASA ADS] [CrossRef] [Google Scholar]
Sambruna, R. M., Eracleous, M., & Mushotzky, R. F. 1999, ApJ, 526, 60 [NASA ADS] [CrossRef] [Google Scholar]
Sambruna, R. M., Reeves, J. N., Braito, V., et al. 2009, ApJ, 700, 1473 [NASA ADS] [CrossRef] [Google Scholar]
Sambruna, R. M., Tombesi, F., Reeves, J. N., et al. 2011, ApJ, 734, 105 [NASA ADS] [CrossRef] [Google Scholar]
Snedden, S. A., & Gaskell, C. M. 1999, ApJ, 521, L91 [NASA ADS] [CrossRef] [Google Scholar]
Tombesi, F., Sambruna, R. M., Reeves, J. N., et al. 2010a, ApJ, 719, 700 [NASA ADS] [CrossRef] [Google Scholar]
Tombesi, F., Cappi, M., Reeves, J. N., et al. 2010b, A&A, 521, A57 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Tombesi, F., Tazaki, F., Mushotzky, R. F., et al. 2014, MNRAS, 443, 2154 [NASA ADS] [CrossRef] [Google Scholar]
Turner, T. J., & Miller, L. 2009, A&ARv, 17, 47 [Google Scholar]
Urry, C. M., & Padovani, P. 1995, PASP, 107, 803 [NASA ADS] [CrossRef] [Google Scholar]
Ursini, F., Petrucci, P. O., Matt, G., et al. 2018, MNRAS, 478, 2663 [NASA ADS] [CrossRef] [Google Scholar]
Vestergaard, M. 2002, ApJ, 571, 733 [NASA ADS] [CrossRef] [Google Scholar]
Wandel, A. 1991, A&A, 241, 5 [NASA ADS] [Google Scholar]
Wilms, J., Allen, A., & McCray, R. 2000, ApJ, 542, 914 [NASA ADS] [CrossRef] [Google Scholar]
Worrall, D. M., Giommi, P., Tananbaum, H., & Zamorani, G. 1987, ApJ, 313, 596 [NASA ADS] [CrossRef] [Google Scholar]
Wozniak, P. R., Zdziarski, A. A., Smith, D., Madejski, G. M., & Johnson, W. N. 1998, MNRAS, 299, 449 [NASA ADS] [CrossRef] [Google Scholar]
In the text
ePUB (4.454 MB)
Simbad Objects
XMM-Newton spectrum of the radio-loud quasar 3C 215: Slim accretion disk or SMBH binary
Broadband spectral analysis of MXB 1659−298 in its soft and hard state
BeppoSAX spectroscopy of MR 2251-178: A test for ionized reflection in radio quiet QSOs
Spectral analysis of the dipping LMXB system XB 1916-053
The Phoenix galaxy as seen by NuSTAR


With its large surface area and round sides, this frying pan can hold in heat and prevent liquids from splattering. Its sloped sides make it easy to toss food or turn it with a spatula. The stick-resistant stainless steel construction allows for even heating and excellent performance.
Premium tri-ply stainless construction distributes heat evenly.
Superior stick resistance with starburst finishing on stainless interior.
Log in or Request an Account to view the estimated shipping rates.
Loyalty Source is a wholly-owned division of KLF Media Inc.


Our first destination wedding at Temecula Creek Inn. We had so much fun preparing for their special day over the 18 months of planning. It was fun being guests and floral designers for this sweet friend.


Service Catalog is often used with Portfolio.
Service Catalog items can be used as Top Results content items, and should show up on the built-in "Services" page (see "Listings page" below).
If you want to categorize your services, you must add some categories to the Services taxonomy first. On the dashboard, you will see a section titled Administer taxonomy. Using the links in the section you can add and edit terms in all of your site vocabularies.
Click the "Add new category" link in the table row for Services.
You will be on the add term page. Add a title and an optional description. When you save, you may be redirected back to the dashboard.
Any site builder can create new terms in all vocabularies, including Services.
On the dashboard (admin/dashboard), click the Service link in the Create Content section.
Or, find the Add Service link in the admin menu along the top of the page.
Enter a title, and add a description. Upload an image to the Icon field if desired. Check the appropriate boxes under the Service category label to assign categories. If you have added any sitewide topics, you can check boxes for those under the Topics label.
Body: Enter a description of the service.
Icon: If desired, upload an icon to represent the service. Icons will be displayed at 48x48px. Because the icon may be used as a link to the service page on various service listings, you must add alt text for the icon.
Service link: If the service is available online, you can add a direct link to its location.
Service category: If you have defined any service categories, you will be able to tag the service with them.
Topics: If you have defined any sitewide topics, you will be able to tag the service with those topics.
Service Catalog provides a basic listings page. Visit /services to see it.
Services are filterable by keyword and by category.
By default this page is not in any menu. To add it, use the Manage Links link on your dashboard for the menu where you'd like it to appear.
There are several widgets available that allow site visitors to either search for Services or view Services. To find these widgets, select "Service Catalog" from "Add Existing Content".
From there, click the "Add" button for either "Services Search Box", "Services Search: Services results", or "Service Catalog: Full listing."


"The Rainier Oven Building is a testament to the idea that time's discrete but pivotal role in creative practice should be considered when we look for ways to build and maintain hubs of space, place, and culture—that planning for and protecting the longevity of creative spaces is important.
Issue 33.3 is printed in two-color on uncoated stock. The issue was designed by Schema.


As a Digital Media Agency we cover multiple aspects of digital marketing, take a look at the full list of our services below.
We offer a wide range of photo and video services for indivuduals and businesses.
Create the perfect website for your business and have it hosted with us today!
Having an issue on starting up? Speak with us and find out how we can help you.
Speak with experts on how to improve your businesses search ranking.
Take a look at our special offers currently available, all of these are subject to staff availability and terms and conditions.
Send us the plans for your artwork and have the first draft completed within 24 Hours.
Choose from a premium template and receive web hosting and CPanel Email.
Need to build traction in your business? Our team will post on social media for you!


Do you have enthusiasm and an enquiring mind?
Do you want to extend your network and enhance your leadership skills?
Do you want to help people become the best that they can be?
If you answered 'Yes' to any of these questions then West Lothian College Board would love to hear from you.
We are currently looking to recruit at least 2 new voluntary Board Members who would be part of a team of 18 working together to ensure that West Lothian College delivers the best learning experience for adult learners and the growing number of young people in the region.
You may never have considered a board position before, but your experience may be invaluable. Public sector boards are very keen to increase the diversity of their non-executive directors so this may be a great opportunity for you.
Many of us don't realise how much we have to offer an organisation, so even if you are not really sure if the boardroom is for you, please do get in touch and we will be able to explain more.


The cash, life, and fuel are infinite.
RouteZ Hacked unblocked is an action game in which you have to drive to survive. You are trapped in a world filled with dangerous monsters. Clean them and you will win. Aside from that, you need to search for fuel and ammo by clearing hordes of zombies. With the car that you have, you can kill every undead on the road. Collecting the coins is useful for you to buy improvements or upgrades. Let's start the engine and get prepared for a fierce battle now!


Book "Little Princes writer Conor Grennan" description: One Person Can Make a Difference In search of adventure, twenty-nine-year-old Conor Grennan traded his day job for a year-long trip around the globe, a journey that began with a three-month stint volunteering at the Little Princes Children's Home, an orphanage in war-torn Nepal.
Wheels for the World! – LA Kelley Communications Inc.
A summary of Chapters IV�VI in Antoine de Saint-Exupery's The Little Prince. Learn exactly what happened in this chapter, scene, or section of The Little Prince and what it means. Perfect for acing essays, tests, and quizzes, as well as for writing lesson plans.
Save One Life is a Massachusetts-based international nonprofit that provides direct financial aid to impoverished people with bleeding disorders in developing countries.
The riveting story of Conor Grennan's year in Nepal reads like a cross between Into Thin Air and Three Cups of Tea. While volunteering at an orphanage, Conor discovers that the children are not orphans: they are trafficked. Despite the danger, Conor treks up dirt paths with photographs of the children, miraculously reuniting dozens of families.


text:
Marla Maples says ex Donald Trump's presidential campaign has made her life 'crazy' as she prepares for 'DWTS'
By Nicki Gostin
Maples will be on the Season 22 of "DWTS" which starts on Monday. (Craig Sjodin/ABC)
Marla Maples is trying to quick-step her way out of questions about her ex-husband Donald Trump's presidential campaign.
The former beauty queen says it's nice to focus on her upcoming stint on the ABC reality competition "Dancing with the Stars" than her orange-hued ex.
"Dancing with the Stars" has given me an opportunity to really be seen in my own light," she says in a clip from the upcoming season obtained by Us magazine.
The new First Family: A look at Donald Trump's family tree
The 52-year-old blond married Trump, 69, in 1993 after reportedly starting an affair while he was still married to his first wife, Ivana. They are parents to a 22-year-old daughter, Tiffany.
Even though she's moved on, Trump's presidential bid has turned Maples life upside down. She's electing to avoid the subject.
Marla Maples and Donald Trump in 1994. (JOHN BAZEMORE/AP)
"It's been a crazy six months for me," Maples explained. "I've had people constantly coming to me, wanting my opinion about the presidential race, and I've maintained a lot of privacy. But now that I'm stepping out and [going to) be a part of 'Dancing with the Stars,' it's intensified even more."
Maples will be partnered with pro Tony Dovolani on the new season of "DWTS," which premieres Monday at 8 p.m.
marla maples
Matt Lauer's wife files for divorce almost two years after sexual misconduct allegations

redpajama_set_name: RedPajamaCommonCrawl


Premium WordPress themes are based on a robust framework. The Virtue Premium has a clean, modern design, powerful options and an appealing layout. It is a powerful, feature-rich, free WordPress theme. The Avant is a highly customizable, multifunctional WordPress theme.
Also, client services have a big influence on my sucess with the topic.
Also, client services have a big influence on my sucess with the topic. Walking Premium was an outstanding option, and I'm sure I'll make it again in the near term. The payment of a WordPress topic is definitely rewarding - especially if you are not a real technician. This rationalizes the construction of a website and thus helps to save a lot of valuable resources.
Wintersfell is a WordPress topic with a clear, minimalistic and fast reacting style, nice gallery..... The Revoke is a premium Wordpress themes with a clear, contemporary and appealing look. The Shape is a photography WordPress subject with clear, minimalistic and reactive designs, nice art gallery and..... Volcano is a WordPress topic with a clear, minimalistic look, soft transitions, and enhanced functionality.


text:
Q: Testing Events and Mail in Laravel 5.2 I am struggling to handle test of an event within a class and a mail call. Is there an alternative to what Laravel 5.5+ comes with, Mail::fake() and similar, within Laravel 5.2?
Here is an example test class
<?php

namespace tests\SampleTest;

use tests\TestCase;
use App\Foo\Bar;

class BarTest extends TestCase
{
    public function testBar() {
        $class = new Bar();
        $class->methodWithEvent();

        // Event is called. Inside event we call Mail
        $this->expectsEvents(App\Events\BarEvent::class);
    }
}

Example Bar Class
<?php

namespace App\Foo;

use App\Events\BarEvent;
use Event;

class Bar
{
    public function methodWithEvent()
    {
        Event::fire(new BarEvent());
    }
}

Example Event File - a default Event File
Example Listener File - handler method
public function handle(BarEvent $event)
{
    $emailData = [
       'from' => 'test@hotmail.com',
       'email' => 'joe.doe@hotmail.com',
       'title' => 'Test'
    ];

    Mail::send('Test Message', ['html' => 'HTML Message'], function ($mail) use ($emailData) {
        $mail->from($emailData['from']);
        $mail->to($emailData['email'])->subject($emailData['title']);
    });
}

A: You can use a Email Capture service like MailTrap to help test emails. If you configure your PHPUnit to use your MailTrap SMTP details, all test events can be captured by MailTrap.
Alternatively, you can set the mail driver to log so that it's not actually send to the email address, but captured in the Laravel log file.
Laravel 5.2 also supports the pretend configuration. If you set MAIL_PRETEND in your .env file to true, Laravel doesn't send out any emails.

redpajama_set_name: RedPajamaStackExchange


text:
College Savers Jumping to Other States' 529 Plans
Not too long ago, if you wanted to use a "Section 529" college savings plan, and your state didn't offer one, you were out of luck. That's no longer the case. Forty-six states now have these college investment programs and more than one-half of them are open to nonresidents.
"This is a wonderful development for families looking at ways to save for their children's college education," says Joseph Hurley, author of "The Best Way to Save for College – A Complete Guide to Section 529 Plans". The states are making these programs as attractive as possible, and with all the choices now available "most people can find a plan that meets their needs," says Hurley.
Federal tax law allows states to design tax-deferred investment programs that are open to everyone no matter what their age or income level, and to accept enough money to pay for the entire cost of a college education. Many parents and grandparents are attracted to 529 plans because they shift the income into the student's tax bracket without risking the loss of control of funds, unlike Uniform Gifts to Minors Act accounts.
"I know some people who are putting hundreds of thousands of dollars into 529 plans," says Hurley. "It's just a great way to save for college."
Hurley maintains information and ratings of the various state programs on his website at www.savingforcollege.com.


text:
Sometimes Bigger Really is Better
Minicars Perform Worst in Frontal Crash Tests
Although the new minicars gaining worldwide popularity may outperform standard sized vehicles in a parallel parking competition, according to new crash test data, these sub-compacts do not measure up to their larger-sized counterparts when it comes to safety.
The Insurance Institute for Highway Safety recently put 11 new minicars through a series of frontal crash tests. Only one of these minicars received an "acceptable" rating, making the vehicles "the worst performing group of any evaluated so far."
The crash test, also referred to as a "small overlap" or "small front overlap," simulates what occurs when the front corner of a car hits another vehicle or stationary object at 40 miles per hour. These type of crashes typically make up nearly 25 percent of all serious or fatal injuries to front-seat occupants in traffic accidents.
The reason for the extremely dismal safety ratings? In seven of the 11 minicars tested, seatbelts failed to hold crash test dummies in place, or airbags proved less than fully effective. In one of the minicars, the airbag did not deploy at all.
Source: Most new "minicars" fail frontal crash tests." Cbsnews.com. January 22, 2014.


There cannot be one true believer in the New Revelation, who would not also fully recognize and receive the teachings of the Scriptures. But most Christians of our time, believing or not in the doctrine of Sola Scriptura, would probably deny without any scruples the New Revelation.
So, to speak against Jesus Christ and implicitly against Christianity can be forgiven, but to speak against the spirit of love, thus to oppose it, cannot ever be… For to be against love means already to condemn yourself in your heart, to put yourself willingly outside the universal order of God and ultimately, to fight against your own fundamental life.


Lady and the Blog → Contest → Start Working On Your Summer Tan Today With Suave Visible Glow PLUS A GIVEAWAY!!
Start Working On Your Summer Tan Today With Suave Visible Glow PLUS A GIVEAWAY!!
Hooked. Hooked. And hooked! Now that I am in my 30s, sunbathing is just not an option. I've learned one too many things about the sun I cannot ignore. If I go to the beach, you will find me under an umbrella or with LOTS of sunblock on for SURE.
But I still love a good tan. Suave® Professionals Visible Glow™ Self-Tanning Body Lotion is my new solution! I keep a bottle in the bathroom and apply the lotion twice a day. I actually keep it on my sink because then I remember to do it.
I've also been traveling quite a bit and bought a second bottle to add to my travel accessories bag. Yes, I have a bag of beauty goodies that is an exact replica of everything I use on a day-to-day basis. Dry shampoo, concealer, deodorant, moisturizer – you name it and I have a double in my travel bag. Suave® ProfessionalsVisible Glow™ has officially been added to that mix.
Friends have been complimenting me as well! And once they hear how easy it is to start working on their summer tan, they start their very own routine. Love it! In 2014, you can't ignore all the negative effects sunbathing has on your skin. Why take the risk?!
I use Fair to Medium because I am very light skinned. After two weeks, it didn't turn me orange or leave any streaks. It was a clean, even darker tone and I was so happy with the glowing results!
Guess What?! I Have A Contest Of My Own!!
I usually use an instant tanner and always get streaks! Thanks for the review!
I'm embarrassed to admit I love a good tan, but usually only get one by being in the sun with no sunblock. Shame on me! Self tanners always smell so bad, but I've heard good things about this Suave one, so I'm thinking of giving it a try!
I love being tan. It makes me feel so much more attractive. I however get this tan by being out in the sun without sunscreen around a swimming pool. Not very healthy!
I generally burn when I try to tan. I usually use sunless tanner.
I've never had the tan I wanted. I would love to try Suave Visible Glow.
I love the look of a tan, but I don't often have one because of UV exposure. I use sunscreen regularly.
I like to be tan because it highlights my eyes and makes me look healthier.
I do like when I'm tan because I feel my clothing looks better. I haven't had time to lay out in the sun to tan with having to chase my kids around. So a tan in a can is my best bet!
i love being tan. self tan!
i like being tan i usually get tan from sitting by the pool.
I love being tan because it makes me look thinner! I've started using tanning lotion on my legs to be capri and gym ready!
I love having a tan. I usually get mine from working in the yard.
I am as white as they come & I would love to try this Suave self-tanner:) I usually just stay out of the sun since I usually burn easy..thanks.
I love being tan. I usually burn to death, then tan. I am half Irish and really white lol.
I like to tan, but I an totally anti-tanning bed. That's why I love this type of product…perfect!
I use sunless tan products because real tans are too damaging for the skin.
I would love to be tan, but I've been too afraid of the side effects… This looks like a great solution. Thanks for the chance to win!
I like to gradually tan outside.
I normally try to tan sunlessly to avoid sun damage to my skin. I do like to tan naturally on occassion like when I'm vacationing at the beach.
I usually get a light tan during the summer but othewise I have that pasty look the rest of the year. I could definitely use this product.
I do not try to tan anymore by sun or salon but I do like to use a self tanner. I usually do a nice mild shade.
I'm African American so I don't need to tan lol But this would be for my best friend. She loves being tan but does not tan easily at all.
I love being tan but am avoiding it because of skin damage 🙁 I have started using sunscreen and self tanner.
I love being tan, and I use to tan years ago in the tanning bed. I have laid off of it, I am in the midst of trying tons of new self tanners!
I like to be tan because it makes my legs look better in dresses. However i'm fair complected so I don't tan well and of course now I know that it isn't safe to lay in the tanning bed.
I absolutely love being tan. I feel way more confident about myself when I am. However I was going about getting tan the wrong way by going to tanning beds. Now I spend some time out in the sun and that is it.
I typically use the Jergens flow stuff to get a little bit of a tan look on my arms and legs. Either that or just go out and do yard work. I try not to stay out in the sun too long though..for health reasons. Thanks for the opportunity to win..I'd love to try these Suave products.
I would love to be tan but I burn instead.
i like to be tan but i don't do anything to get tan yet. i am tony l smoaks on rafflecopter.
I do like being tan.
I do like being tan, but don't want wrinkles so I use self tanner.
I am lucky that I was blessed with naturally dark skin so I don't have the need to "sunbathe", but it's really nice to add an extra glow for special occasions !!
I love being tan! I get my tan during the summer.
I like being tan, but most of the time I am really white. Sometimes I use self-tanning lotions.
I'm normally super pale but I love being tan.
Thanks for the giveaway…a tan is part of living in desert southwest, but we still use sunscreen year-round !


Mandy Leone as Julie B.
Merrit Sander as Roxanna, same girl?
Sorry but we don't have any suppliers for this title. If you're interested in buying Vibre Oh ma soeur please try using a search engine to locate a copy or, failing that, ask for assistance on our main forum. Please DO NOT email us directly for assistance as we simply don't have the time to answer any such requests for help.


text:
Next Wave #854: The Regrettes
Rita Ora Is The Fourth Face Of Issue 109
Robin Murray /
Clash first encountered The Regrettes in 2016, around the time the outrageously precocious Los Angeles group were working on their debut album 'Feel Your Feelings Fool!'. "The Regrettes kick serious ass," we said, and thankfully we've been able to stick around and see that, almost literally, happen.
In town for a quickfire show at the Old Blue Last, singer Lydia Night – still in her teens, but worldy-wise and eloquent in such a succinct manner – hits us up via the phone in her West London hotel room.
"I love the UK and I love London," she tells Clash. "I try to wake up as early as possible and I walk and explore as much as I can. There are so many different little parts that are amazing. I love the food. The parks are my favourite."
Still incredibly young, Lydia wants to experience as much as she can, grabbing each moment and wrestling it down to the ground. It all merges with her songwriting, that vulnerable life-force which fuses punk energy to a clear taste for pop melody.
"I mean, a lot of times my songs are written from a super-personal, vulnerable space," she admits. "Sometimes it is fun to experiment and write from an outside perspective, or even write from the viewpoint of a character. It becomes a fun fiction thing. So I like doing both."
Recently heading out in the desert of the Joshua Tree area in California, The Regrettes have begun to sketch out their new album. Yet drummer Maxx Morando won't be participating, having left the band – amicably, we must point out - on the eve of their European tour.
"Our new drummer is incredible," she gushes. "As a human and as a drummer. This is our first tour with him. And the energy has totally shifted so it's a new beginning. At first that's really scary, because change is always really scary in the beginning, but it's been for the better."
Playing live is absolutely key to the band, who will kick off another coast-to-coast American route once their European itinerary comes to an end. It's here they burst into full bloom, the jagged edges of their songwriting allowed to cut down all before them. "I think that all the songs take on a new life when we play them live," she insists. "We don't really get bored of them. It just feels different. It's weird, it's crazy how that happens. You play the songs so many times and we haven't gotten sick of 'em. Which is crazy."
There's also a pop edge, a word Lydia isn't afraid of using. "I think it's what you make of it," she argues. "I think a lot of people assume now that pop is like Top 40 which I don't agree with. When I think of pop I think of hooky melody, and really catchy riffs. I think of rock bands that have pop elements. I don't think it's a bad word at all."
"I write so much," Lydia continues. "I would feel weird writing so much and not releasing music as often as possible and getting it out into the world. It would feel like I was holding things back from our fans. It's like, there's this song, and people should hear it."
With The Regrettes set to return to the UK for a short headline burst ahead of their much-anticipated Reading and Leeds slots, Clash can't help but ask if the band will be dropping in anything new for fans during those performances.
"Hmmm," she purrs; "Maybe… Wouldn't be a surprise if I told you!"
The Regrettes
Next Wave #937: Glowie


The PES team, based at the Advanced Manufacturing Park (AMP) Sheffield have experience of utilising additive manufacturing within the design process as a material and also a solution and application in other engineering design projects.
Design for manufacturing (DFM) has typically meant that designers should tailor their designs to eliminate manufacturing difficulties and minimize costs. However, the improvement of rapid prototyping (RP), or Additive Manufacturing (AM), technologies provide an opportunity to re-think DFM to take advantage of the unique capabilities of this technology.
Due to the advances of additive manufacture (AM) technologies, it is now being commonly used as a final solution for small batch manufacture and not just for models or prototype evaluation. This technology and process is now being used in multiple sectors including medical, aerospace and fabricated moulds to name but a few.
Shape complexity: it is possible to build virtually any shape, lot sizes of one are practical, customised geometries are achieved readily, and shape optimization is enabled.
Material complexity: material can be processed one point, or one layer, at a time, enabling the manufacture of parts with complex material compositions and designed property gradients. It should be noted new materials are being developed almost on a weekly basis.
We consider all projects regardless of size or complexity and 70% of our clients are internationally based so do please call us for an informal chat. Whether a quick turnaround, simple tooling or modelling job, to complex design engineering projects. We will be able to deliver you a solution.
Additive Manufacturing (AM) technologies, enable the fabrication of parts and concepts that are geometrically complex, have graded material compositions, and can be customised.
Whilst the knowledge and principles developed in design engineering are critical in any design, this technology has added a new dimension which can lead to designs that are very geometrically complex and outside of the traditional design thinking.
The unique capabilities of AM technologies enable new opportunities for pushing design boundaries and customization, very significant improvements in product performance, multi-functionality, and lower overall manufacturing costs.
In order to take advantage of AM capabilities, new design and CAD methodologies must be developed. Design for Additive Manufacturing (DFAM) which is similar to DFM principles, has a similar end result, the process and applied design thinking is very different from the traditional route.
The PES team design methodology is based around process-structure-property-behaviour and we can support and help you to design and develop a new concept or optimise a current design.
We can help to develop a solution for you and look at the opportunities of applying AM as a solution to your design challenges.


Lock in a great price for Hotel Escapade – rated 8.4 by recent guests!
Comfy beds, bathroom with toiletries, hairdryer.... Very good dining for evening meal. Breakfast has all you need , good choice.
Very friendly staff, a warm welcome in this pleasant family hotel. Location is great, just off the beach. Super clean room with a comfortable bed and a good buffet breakfast with fresh local products - bakeries, cheese. Well suited for staying with small children (and dogs, if interested). Good wifi connection.
Delicious buffet breakfast with the facility to boil eggs or fry bacon and eggs yourself. Good coffee. Staff very friendly, efficient and accommodating. Our room was spacious with everything we needed. Very comfortable bed. Great location too. Really enjoyed our stay here.
Nice hotel - very close to the beach. Easy to park (at least in March!). Very helpful staff - provided a baby chair in the restaurant for breakfast. Room is reasonably large.
Super quick check in and check out, friendly staff, excellent location : the beach is only 140 meters from the hotel, several restaurants in walking distance (we dined in the Bistro Carnac, excellent) because the hotel restaurant (which has an excellent reputation as well) was closed during low season. Our room was clean and spacey and quiet, bathroom with plenty of amenities, good shower temp regulation. Excellent breakfast with friendly and attentive staff. We'll be back for sure!
Very friendly staff. Near the beach. My second visit at this hotel.
Room was very light, 4 patio type windows with 4 small balconies. Nice large size flat screen TV. Bed was very comfortable. Loved the bathroom with big window. Charlie, my dog stayed for free!
One of our top picks in De Haan.Hotel Escapade is 250 feet from the beach and within walking distance of the woods. This is an ideal point to start your walk or bike trip. The restaurant will serve you delicious French and regional food. Hotel Escapade features all the facilities for an unforgettable vacation.
De Haan is a quiet and peaceful vacation spot. The hotel is less than 12 miles from the historic city of Bruges and from Ostend.
There is a coastal tram service providing easy connection between De Haan and other seaside cities such as Ostend and Blankenberge.
When would you like to stay at Hotel Escapade?
This room features a spacious bathroom with a shower.
Cable TV and a bathroom with a shower come standard in this room.
A spacious room with a private bathroom has a shower.
This room includes a double bed and 2 single beds. It includes a bathroom with a shower.
House Rules Hotel Escapade takes special requests – add in the next step!
Hotel Escapade accepts these cards and reserves the right to temporarily hold an amount prior to arrival.
Please note that during July and August there is no check-in possible before 13.00.
The parking space at the hotel is limited for 5 cars only.
Please note that the restaurant is open during school holidays.
Room was a bit small, especially the shower cabin. Price of the room a bit too steep for what it was but possibly that was because we visited during a public holiday weekend.
Hotel car park only has space for 4 or 5 cars so you have to park on the street. However, it was free and we found a space easily, but this might be more difficult in high season.
The room was a bit noisy, facing the street - the sound insulation wasn't the greatest and our neighbors woke me up when they came back from the restaurant.
Beds less than comfortable, but mattresses due to be replaced.
Good location. Excellent breakfast. Friendly and efficient owners. Very pleasant bedroom and good en suite bathroom.
Parking but depends on time of year for spaces in the area.


Today I attended Heartstrings: The Leukemia and Lymphoma Society 2013 Saint Valentine's Day Luncheon and Fashion Show (THAT's a mouthful!) at the Meyerson. I was thrilled to be seated next to my pal, Jane McGarry, who snapped this photo of the two of us (Sorry Jane! I had to cut you out for this posts purpose!) and posted it to her social channels. Someone on Facebook commented on the photo to let me know that Jordin Sparks had worn this BCBG Elouise Print-Block Sheath dress the night before on Joan River's Fashion Police on E!. I'm not even going to ask you people to comment and tell me "who wore it best", because I am not a glutton for punishment. Jordin's 20 years my Junior and cute as a button. Let's just say, we each brought something special to the dress and leave it at that... shall we?
Thanks to BCBG for styling me for this event. The Elouise Print-Block Sheath dress and Harlow Leather Envelope Clutch can be purchased at BCBG at NorthPark Center or online.


text:
The Grown Ups — Book Review
I have lived a great deal among grown-ups. I have seen them intimately, close at hand. And that hasn't much improved my opinion of them.
Antoine de Saint-Exupéry, The Little Prince
They had entered the thorny wilderness, and the golden gates of their childhood had for ever closed behind them.
George Eliot, The Mill on the Floss
What does it mean to be a "grown-up"? That's one of the questions that Robin Antalek asks in her engaging coming-of-age novel, The Grown Ups. The book opens in the summer of 1997, with Suzie Epstein, Sam Turner, and their friends celebrating Suzie's fifteenth birthday at a loosely supervised party in Rye, New York. That night, Suzie and Sam embark on a clandestine romance that will last all summer.
Right away, we know something is not right in the neighborhood: "It was the summer all the children in the neighborhood caught a virus." Soon it becomes apparent that the grown-ups have more serious problems than the stomach flu: "The second time Mr. Epstein caused a scene in the driveway of the Epstein family home, the neighborhood was still under siege by the virus and was unusually quiet for the middle of a summer day."
The Epsteins' marriage is not the only troubled one in the neighborhood. Later in the summer, Sam's mother abandons her husband and sons, leaving suddenly with no explanation. Suzie's family moves to Boston, where her mother's alcoholism and her father's philandering escalate. She becomes the adult in the family, caring for her mother and her two younger brothers. Suzie desperately misses her old friends in Rye, especially her best friend, Bella Spade; out of embarrassment, she doesn't answer their letters or phone calls.
When Bella's mother dies of a long and mysterious illness, the old friends, now college juniors, all reunite at her funeral. Suzie, to everyone's surprise, arrives on the arm of Michael Turner, Sam's brilliant and accomplished older brother. Sam, who's had an on-again, off-again relationship with Bella, is surprised at the emotions Suzie evokes. The remaining three-quarters of the book focuses on the relationships among Sam, Suzie, Bella, and Michael, as they struggle to succeed as fully functioning, emotionally healthy adults.
Sam, in particular, fumbles his way through life, unable to commit to anyone or anything. His kindhearted father, Hunt — one of the few responsible and stable adults in the novel — shows admirable patience as Sam repeatedly makes bad decisions. Sam understands the depth of his father's support: "If ever he had any illusion that he could survive in the world without his father, Sam was dumber than he already felt." Of course, like all children, Sam will one day have to survive without his father's love and guidance; isn't that what being "grown up" is all about?
Sam is by far the most interesting and well-developed character in the novel. In an interview on Albany Public Radio, Robin Antalek says her early drafts of the book were narrated by Sam. Later, she rewrote The Grown Ups in the third person, adding the viewpoints of Suzie and Bella. The multiple perspectives add texture and depth to the book, but Suzie and Bella don't come alive the way Sam does.
Some of the details in the novel seem inappropriate to the era. For example, the description of the mothers' activities — hanging laundry outside, smoking cigarettes on their front stoops –sounds more like a description of housewives in the early sixties (the Madmen era) than in the late nineties. I would have appreciated more details pointing to the passage of time — for example, references to new technology or pop culture would underscore the novel's themes of changing and getting older.
Many things happen in 15 years — weddings, funerals, births, illnesses, triumphs and disappointments large and small — and a lot of growing up. The Grown Ups both begins and ends with a birthday party. I don't want to give anything away, but I think it's safe to reveal that the party in the last chapter is very different from the disastrous one in the first chapter:
They were here now, all of them. Relationships slightly rearranged, but still together. That was more than any of them would have imagined years before. They had watched their parents stumble and vowed never to do the same, only to fail one another in entirely different ways . . .
If you enjoyed Meg Wolitzer's The Interestings and/or Jeffrey Eugenides's The Marriage Plot, The Grown Ups will be up your alley.
For more reviews, check out TLC Book Tours.
Posted in Book reviewsTagged robin antalek, the grown ups
Previous Article 10 Favorite Books About Sisters
Next Article WWW Wednesday — Staff Picks
6 thoughts on "The Grown Ups — Book Review"
Julie Valerie @Julie_Valerie says:
Very interesting that Sam was the most developed character in this third person POV book – because earlier drafts were written with Sam as narrator. Makes perfect sense.
Ann@BooksontheTable says:
Yes, very interesting — and I don't think the change was entirely successful. But still an interesting book. I'm always fascinated by a "behind the scenes" look at an author's process. >
This one is totally my thing. Loved The Interestings, too. I must pick this one up.
I hope you enjoy it! Thanks for stopping by. 🙂
Pingback: Robin Antalek, author of The Grown Ups, on tour January/February 2015 | TLC Book Tours
Heather J. @ TLC says:
It sounds like quite a lot changes in everyone's lives between those two birthday parties…
Thanks for being a part of the tour!


The Port of Hueneme welcomed its first vessel in 1941, embarking on an ambitious mission to maximize maritime commerce and provide extensive economic benefits to the community.
Since its inception, The Port's hallmark has been strong leadership. Perhaps that's because all members of the five-member Board of Harbor Commissioners must be voted into office by the citizenry of The Oxnard Harbor District.
Once the officers have been elected, primary responsibilities fall squarely on the shoulders of a CEO, Port Director, and select staff, who administer all policies and operations. Their influence is far-reaching to say the least, as the District's political boundaries encompass the Greater City of Oxnard (population 181,000) and the City of Port Hueneme (population 22,000).
Continuity, of course, is indispensable for the shaping of sound, long-term policies. To ensure the needed continuity, the commissioners' four-year terms are strategically staggered.
The Port of Hueneme is owned and operated by the Oxnard Harbor District, a political subdivision of the State of California. Nevertheless, the bustling commercial gateway remains vigorously independent – a glowing example of a self-supporting business enterprise.
The District is bound by a charter with The City of Port Hueneme. This agreement gives The District complete authority to acquire, construct, own, operate, control, or develop any and all harbor works or facilities. Underscoring its independence, The District prepares and controls its own budget and fiscal activities in order to reach its wide-ranging objectives.
Despite the staggering expenses associated with operating a busy international port, The Oxnard Harbor District collects absolutely no taxes. Operating funds are generated exclusively by Port-related businesses, which enter into highly productive operating agreements with the 'landlord' port. Business-generated revenues in turn enable The Harbor District to fund a variety of support services provided by The City of Port Hueneme.
A pivotal component in the intermodal logistics supply chain, The Port of Hueneme is a major contributor to the economic health of Ventura County and Southern California. The following is a snapshot of The Port's key economic contributions.
Over $9 billion in cargo annually.
$1.5 billion in overall economic impact.
$93 million paid in annual taxes.
Provides more than 13,633 direct, indirect, induced and influenced jobs regionally.
Top trading partners include: Austria, Brazil, Canada, Costa Rica, China, Ecuador, Germany, Great Britain, Guatemala, Japan, Korea and Mexico.


Planning a novel should follow the monomyth.
The character is boring unless they are also wrestling with conflict. The conflict should have a purpose – the character returning to life transformed by it. To maintain interest conflict should start early in the book.
When working out your book plan – planning around 20 chapters is a good average to start with. The plan should include the basic plot which you then use to write the book from.
In previous blog posts we have considered the seven basic plots https://magic-phil.co.uk/2018/01/23/seven-basic-plots/ and the framework of the novel https://magic-phil.co.uk/2018/02/06/the-framework-of-a-novel/. So we have covered the monomyth and the seven basic plots already.
Choose which of the seven basic plots you would like to plan and work out your plot.
Start with the premise of someone who will not/cannot adapt to society.
In what way can they not adapt?
Perhaps they have a sense of isolation –a self-constructed cell that has no walls but which permits no escape.
What kind of a world should it be? Not too different to this one.
It sounds like an illness – what kind of obscure illness should it be?
What are the sanctions to this person? Where/who do the sanctions come from?
Why do they have to hide?
What do they do if they still don't adapt?
What kind of lack of adaptation would cause complete shunning of them by the rest of society?
Where can you run when the whole world is owned? What if the effort to own is too much? Where can you go with that? What if the competition is too much?
As you can see working out the plot causes many questions. I only had time to list some on the course but the longer that you spend the more questions you will have. I also think that having lots of questions will fill better fill out the plot and lead to more interesting characters.
At the age of nine comes selection. Thomas had always regarded himself as different and shuddered now in the line.
He saw the days before as carefree. Days in which games and laughter as much filled the playrooms as the careful instruction to comply, to serve, to address the ills that an unregulated and unconforming world could only bring.
Thomas has been raised like all children (since a time that no one alive would now remember) in a crèche away from interference and distraction. Loved and managed by Nana who's warm smoothness had sheltered them when babies. At night time she ushered them to sleep as they grew.
Nana was the kindest machine Thomas had so far encountered and he loved her as he loved no one living.
Thomas had never felt the same about the others, those his own age with which he shared a nursery, sleeping, eating, playing. To Thomas they were all different, something he always kept closely to himself. Thomas never wanted to fit, he didn't want to be selected, but when he told Nana this she had dismissed it. Everyone had to be conditioned – why wasn't he more like his crèche mates.
He had learned to speak no more of it.
He had wondered if he was special and in darker moments if his parents had been criminals – the few for whom conditioning would not take.
The other children were so happy that they would be allowed 21 days a year to go to the sun, to sit on beaches with other conditioned people. They were happy to fit a normal life, performing their function.
Thomas couldn't imagine any future could be worse – all of life given to a function, no more games, no more Nana.
With the selection he would be one of many allocated to a discipline for which he was best suited. His brain activity analysed, his aptitudes scanned and evaluated, it would not take long – Nana said it wouldn't hurt.
So far Thomas had to agree, it was boring, staring at the back of someone's head. He was wishing in that he would not get taken inside, they'd forget somehow, that he wouldn't have to serve.
The selection booth seemed quiet, apart from a muted background hum. Thomas didn't feel happiness, didn't feel peace. This chamber felt like a threat to him. He felt fear trembling in his legs and thudding with rapid repetition in his chest.
The door behind him closed, there now seemed no way back – only forwards.
He slid to the ground and began to cry, would he have to work? Would he never be able to run around Nana screaming with happiness?
As he sat the helmet levitated from the inner room – the place where he was to arrive – but he had resisted. It passed unseen overhead as he huddled inside the door and descended onto his bowed head. With a puff of anaesthetic the electrodes engaged.
Thomas was conscious of the analysis but felt no need to attempt to dislodge the device. His body now lifted and set in a chair. Electrodes strapped over him reading wishes, desires, aptitudes.
Somewhere behind it all was Thomas. He wanted to avoid allocation, to be without work, to run outside again, free.
The machine reading the purpose for which he was best suited. It engaged the first stage of programming – coercing the mind into a path which was most suitable.
It hadn't taken long. Thomas emerged now. A technician – training downloaded, programming embedded. He was ready for a contented life in service, keen to embark on a lengthy apprenticeship to fulfil his true purpose.
Machines are not perfect. The design of the programming helmet is to smooth neural pathways. It is to direct the growth of learning and to remove old memories. In fact to remove anything that would hinder the future happiness of those who came within its attention.
Outwardly Thomas was now a keen young technician destined as he was for 10 years of training, acclimatization and conditioning. Life much easier than ever before: regular breaks, true holidays and downtime. He was programmed to meet those which similar machines had designated appropriate. With some of whom Thomas could produce future generations of adapted technicians.
Thomas had the neural seeds of discontent sowed within him.
Outwardly the smiling face of just another happy employee but in fact gradually that seed would grow, and each night emerge in dreaming.
The Thomas not in technician's uniform. The Thomas not working at all, running along a rainswept shore. The Thomas unlimited by 21 days of annual leave; the designated holiday-destinations in approved-hotels. The hotels where Thomas would meet with those who reaffirmed the importance of a technician's life.
How vital it was that he put in those 39 hours a week monitoring, maintaining, fabricating.
Hidden to those around him, Thomas' growing awareness that this life was not for him.
This is just the intro to the process which might give you a few pointers but as you can see there is quite a bit more to it.


Our product range includes a wide range of garlic flake, garlic granules, ginger garlic paste, potato starch, dehydrated garlic and dried garlic granules.
We ensure the quality of Garlic Flake to our valuable clients. The dehydrated garlic flake have excellent flavor and taste that is similar to the fresh garlic. We offer the dehydrated garlic flake at economical prices. These are highly in demand for their best quality in market.
We are leading manufacturer & exporter of Garlic Granules and our product is made up of good quality.
We are leading Manufaturer of Ginger Garlic Paste and our product is made up of good quality.
We are leading Manufaturer of Potato Starch and our product is made up of good quality.
These Dehydrated Garlic are highly appreciated by our client for their rich taste and purity. These are easily available at very reasonable price in market. The dehydrated garlics is free from any added artificial coloring matter.
Being one of the eminent names of the business, we bring forth Dried Garlic Granules. Free from preservatives, the offered garlic granules are quite suitable for making garlic breads and can be added in burgers, salads & French fries too. Dried garlic granules are stored in a cool dry place and can remain fresh for a long time. These granules are vastly popular for their fine nutritional value and excellent taste.
We are concerned with the manufacture and trade of Dried Garlic that is processed at a certain temperature. Added to burgers, rice, mushroom soups, pizzas and other food items, this garlic powder is widely appreciated for its amazing flavor and high nutritional value. Dried garlic is provided in airtight packaging and can be stored for a longer time period.
We bring forth for our clients an extensive range of Dried Garlic Powder. This is processed under the supervision of highly skilled & adroit chefs using superior quality ingredients under hygienic environment so that it can be stored for long.
We are leading Manufaturer of Frozen Garlic and our product is made up of good quality.
Leveraging upon our rich domain expertise we are engaged in offering a wide range of Ginger And Garlic Mixed Paste.
With a vision and keenness to provide healthy and highly nutritious product to our customers, we present natural sweetener in the form of Garlic Paste that is used for making meat, chicken and other such dishes.
We are among the pioneers in the industry for manufacturing and supplying No Skin Garlic to our revered patrons. The offered cloves are demanded in food processing industry and restaurants.
We are offering a wide gamut of Onion Garlic Ginger Paste to the clients. These products are processed with the help of organic ginger and garlic. These products are used for preparing food items in the different kitchen.
We are a reputed entity in the industry, actively engaged in offering an optimum quality range of Fresh Garlic Paste.
Owing to our skilled team of professionals, we have emerged as a renowned firm of an assorted range of Peeled Fresh Garlic.
We are engaged in proffering Dehydrated Garlic Flake, which has a pale yellow to light brown color. With characteristic pungent and zero contaminants, the offered garlic flakes are widely known for its pungent flavor. Demanded for adding flavor in dry soups mixes, sauces, vegetable mixes, stuffing mixes and fast foods, the offered garlic flakes are vastly sought after.
We offer our customers with best quality Beet Root Powder that are rich in taste and flavor. We offer these Dried Beet Root Powder in various specifications and ensure the packaging is done in an effective manner to avoid wastage during transportation.
Owing to our expertise in this domain, we are engaged in manufacturing and supplying optimum quality Lemon Powder that helps in cases related to poor digestion and sinus. Our provided lemon powder is hygienically processed using the finest quality lemon and ultra-modern technology under the supervision of our skilled professionals. The offered powder is tested by our team of experts on various quality measures.
We are successfully meeting the varied requirements of our clients by providing the best quality range of Ginger Paste.
We are reckoned as one of the preeminent Dehydrated Garlic Manufacturers and Exporters from India. The panchvati foods take meticulous measures to ensure an outstanding Dried to Eat Garlic.