Measurement of Galactic synchrotron emission

# The angular power spectrum measurement of the Galactic synchrotron emission in two fields of the TGSS survey

Samir Choudhuri, Somnath Bharadwaj, Sk. Saiyad Ali, Nirupam Roy Huib. T. Intema and Abhik Ghosh
National Centre For Radio Astrophysics, Post Bag 3, Ganeshkhind, Pune 411 007, India
Department of Physics, & Centre for Theoretical Studies, IIT Kharagpur, Kharagpur 721 302, India
Department of Physics,Jadavpur University, Kolkata 700032, India
Department of Physics, Indian Institute of Science, Bangalore 560012, India
Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333CA, Leiden, The Netherlands
Department of Physics and Astronomy, University of the Western Cape, Robert Sobukwe Road, Bellville 7535, South Africa
SKA SA, The Park, Park Road, Pinelands 7405, South Africa
Email:samir11@phy.iitkgp.ernet.in
###### Abstract

Characterizing the diffuse Galactic synchrotron emission at arcminute angular scales is needed to reliably remove foregrounds in cosmological 21-cm measurements. The study of this emission is also interesting in its own right. Here, we quantify the fluctuations of the diffuse Galactic synchrotron emission using visibility data for two of the fields observed by the TIFR GMRT Sky Survey (TGSS). We have used the 2D Tapered Gridded Estimator (TGE) to estimate the angular power spectrum from the visibilities. We find that the sky signal, after subtracting the point sources, is likely dominated by the diffuse Galactic synchrotron radiation across the angular multipole range . We present a power law fit, , to the measured over this range. We find that have values and in the two fields. For the second field, however, there is indication of a significant residual point source contribution, and for this field we interpret the measured as an upper limit for the diffuse Galactic synchrotron emission. While in both fields the slopes are consistent with earlier measurements, the second field appears to have an amplitude which is considerably smaller compared to similar measurements in other parts of the sky.

###### keywords:
methods: statistical, data analysis - techniques: interferometric- cosmology: diffuse radiation

## 1 Introduction

Observations of the redshifted 21-cm signal from the Epoch of Reionization (EoR) contain a wealth of cosmological and astrophysical information (Bharadwaj & Ali, 2005; Furlanetto et al., 2006; Morales & Wyithe, 2010; Pritchard & Loeb, 2012). The Giant Metrewave Radio Telescope (GMRT, Swarup et al. 1991) is currently functioning at a frequency band which corresponds to the 21-cm signal from this epoch. Several ongoing and future experiments such as the Donald C. Backer Precision Array to Probe the Epoch of Reionization (PAPER, Parsons et al. 2010), the Low Frequency Array (LOFAR, var Haarlem et al. 2013), the Murchison Wide-field Array (MWA, Bowman et al. 2013), the Square Kilometer Array (SKA1 LOW, Koopmans et al. 2015) and the Hydrogen Epoch of Reionization Array (HERA, Neben et al. 2016) are aiming to measure the EoR 21-cm signal. The EoR 21-cm signal is overwhelmed by different foregrounds which are four to five orders of magnitude stronger than the expected 21-cm signal (Shaver et al., 1999; Ali et al., 2008; Ghosh et al., 2011a, b). Accurately modelling and subtracting the foregrounds from the data are the main challenges for detecting the EoR 21-cm signal. The diffuse Galactic synchrotron emission (hereafter, DGSE) is expected to be the most dominant foreground at arcminute angular scales after point source subtraction at 10-20 mJy level (Bernardi et al., 2009; Ghosh et al., 2012; Iacobelli et al., 2013). A precise characterization and a detailed understanding of the DGSE is needed to reliably remove foregrounds in 21-cm experiments. In this paper, we characterize the DGSE at arcminute angular scales which are relevant for the cosmological 21-cm studies.

The study of the DGSE is also important in its own right. The angular power spectrum () of the DGSE quantifies the fluctuations in the magnetic field and in the electron density of the turbulent interstellar medium (ISM) of our Galaxy (e.g. Waelkens et al. 2009; Lazarian & Pogosyan 2012; Iacobelli et al. 2013).

There are several observations towards characterizing the DGSE spanning a wide range of frequency. Haslam et al. (1982) have measured the all sky diffuse Galactic synchrotron radiation at . Reich (1982) and Reich & Reich (1988) have presented the Galactic synchrotron maps at a relatively higher frequency . Using the Rhodes Survey, Giardino et al. (2001) have shown that the of the diffuse Galactic synchrotron radiation behaves like a power law where the power law index in the range . Giardino et al. (2002) have found that the value of is for the Parkes Survey in the range . The measured from the Wilkinson Microwave Anisotropy Probe (WMAP) data show a slightly lower value of for (Bennett et al., 2003). Bernardi et al. (2009) have analysed Westerbork Synthesis Radio Telescope (WSRT) observations to characterize the statistical properties of the diffuse Galactic emission and find that

 Cℓ=A×(1000l)βmK2 (1)

where and for . Ghosh et al. (2012) have used GMRT observations to characterize the foregrounds for 21-cm experiments and find that and in the range . Recently, Iacobelli et al. (2013) present the first LOFAR detection of the DGSE around . They reported that the of the foreground synchrotron fluctuations is approximately a power law with a slope up to angular multipoles of .

In this paper we study the statistical properties of the DGSE using two fields observed by the TIFR GMRT Sky Survey (TGSS; Sirothia et al. 2014). We have used the data which was calibrated and processed by Intema et al. (2016). We have applied the Tapered Gridded Estimator (TGE; Choudhuri et al. 2016, hereafter Paper I) to the residual data to measure the of the background sky signal after point source subtraction. The TGE suppresses the contribution from the residual point sources in the outer region of the telescope’s field of view (FoV) and also internally subtracts out the noise bias to give an unbiased estimate of (Choudhuri et al., 2016a). For each field we are able to identify an angular multipole range where the measured is likely dominated by the DGSE, and we present power law fits for these.

## 2 Data Analysis

The TGSS survey contains 2000 hours of observing time divided on 5336 individual pointings on an approximate hexagonal grid. The observing time for each field is about minutes. For the purpose of this paper, we have used only two data sets for two fields located at Galactic coordinates ; Data1) and ; Data2). We have selected these fields because they are close to the Galactic plane, and also the contributions from the very bright compact sources are much less in these fields. The central frequency of this survey is with an instantaneous bandwidth of which is divided into frequency channels. All the TGSS raw data was analysed with a fully automated pipeline based on the SPAM package (Intema et al., 2009; Intema, 2014). The operation of the SPAM package is divided into two parts: (a)Pre-processing and (b) Main pipeline. The Pre-processing step calculates good-quality instrumental calibration from the best available scans on one of the primary calibrators, and transfers these to the target field. In the Main pipeline the direction independent and direction dependent calibrations are calculated for each field, and the calibrated visibilities are converted into “CLEANed” deconvolved radio images. The off source rms noise () for the continuum images of these fields are and for Data1 and Data2 respectively, both values lie close to the median rms. noise of for the whole survey. The angular resolution of these observations is  . This pipeline applies direction-dependent gains to image and subtract point sources to a flux threshold covering an angular region of radius times the telescope’s FoV (), and also includes a few bright sources even further away. The subsequent analysis here uses the residual visibility data after subtracting out the discrete sources.

We have used the TGE to estimate from the measured visibilities with referring to the corresponding baseline. As mentioned earlier, the TGE suppresses the contribution from the residual point sources in the outer region of the telescope’s FoV and also internally subtracts out the noise bias to give an unbiased estimate of (details in Choudhuri et al. 2014, 2016a, Paper I). The tapering is introduced by multiplying the sky with a Gaussian window function . The value of should be chosen in such a way that it cuts off the sky response well before the first null of the primary beam without removing too much of the signal from the central region. Here we have used which is slightly smaller than , the half width at half maxima (HWHM) of the GMRT primary beam at . This is implemented by dividing the plane into a rectangular grid and evaluating the convolved visibilities at every grid point

 Vcg=∑i~w(Ug−Ui)Vi (2)

where is the Fourier transform of the taper window function and refers to the baseline of different grid points. The entire data containing visibility measurements in different frequency channels that spans a bandwidth was collapsed to a single grid after scaling each baseline to the appropriate frequency.

The self correlation of the gridded and convolved visibilities (equation (10) and (13) of Paper I) can be written as,

 ⟨∣Vcg∣2⟩=(∂B∂T)2∫d2U∣~K(Ug−U)∣2C2πUg+∑i∣~w(Ug−Ui)∣2⟨∣Ni∣2⟩, (3)

where, is the conversion factor from brightness temperature to specific intensity, is the noise contribution to the individual visibility and is an effective “gridding kernel” which incorporates the effects of (a) telescope’s primary beam pattern (b) the tapering window function and (c) the baseline sampling in the plane.

We have approximated the convolution in equation (3) as,

 ⟨∣Vcg∣2⟩=[(∂B∂T)2∫d2U∣~K(Ug−U)∣2]C2πUg+∑i∣~w(Ug−Ui)∣2⟨∣Ni∣2⟩, (4)

under the assumption that the is nearly constant across the width of .

We define the Tapered Gridded Estimator (TGE) as

 ^Eg=M−1g(∣Vcg∣2−∑i∣~w(Ug−Ui)∣2∣Vi∣2). (5)

where is the normalizing factor which we have calculated by using simulated visibilities corresponding to an unit angular power spectrum (details in Paper I). We have i.e. the TGE provides an unbiased estimate of the angular power spectrum at the angular multipole corresponding to the baseline . We have used the TGE to estimate and its variance in bins of equal logarithmic interval in (equations (19) and (25) in Paper I).

## 3 Results and Conclusions

The upper curves of the left and right panels of Figure 1 show the estimated before point source subtraction for Data1 and Data2 respectively. We find that for both the data sets the measured is in the range across the entire range. Model predictions (Ali et al., 2008) indicate that the point source contribution is expected to be considerably larger than the Galactic synchrotron emission across much of the range considered here, however the two may be comparable at the smaller values of our interest. Further, the convolution in equation (3) is expected to be important at small , and it is necessary to also account for this. The lower curves of both the panels of Figure 1 show the estimated after point source subtraction. We see that removing the point sources causes a very substantial drop in the measured at large . This clearly demonstrates that the at these angular scales was dominated by the point sources prior to their subtraction. We further believe that after point source subtraction the measured at large continues to be dominated by the residual point sources which are below the threshold flux. The residual flux from imperfect subtraction of the bright sources possibly also makes a significant contribution in the measured at large . This interpretation is mainly guided by the model predictions (Figure 6 of Ali et al. 2008), and is also indicated by the nearly flat which is consistent with the Poisson fluctuations of a random point source distribution. In contrast to this, shows a steep power-law dependence at small () with and for Data1 and Data2 respectively. This steep power law is the characteristic of the diffuse Galactic emission and we believe that the measured is possibly dominated by the DGSE at the large angular scales corresponding to . As mentioned earlier, the convolution in equation (3) is expected to be important at large angular scales and it is necessary to account for this in order to correctly interpret the results at small .

We have carried out simulations in order to assess the effect of the convolution on the estimated . GMRT visibility data was simulated assuming that the sky brightness temperature fluctuations are a realization of a Gaussian random field with input model angular power spectrum of the form given by eq. (1). The simulations incorporate the GMRT primary beam pattern and the tracks corresponding to the actual observation under consideration. The reader is referred to Choudhuri et al. (2014) for more details of the simulations. Figure 2 shows the estimated from the Data1 simulations for and which roughly encompasses the entire range of the power law index we expect for the Galactic synchrotron emission. We find that the effect of the convolution is important in the range , and we have excluded this range from our analysis. We are, however, able to recover the input model angular power spectrum quite accurately in the region which we have used for our subsequent analysis. We have also carried out the same analysis for Data2 (not shown here) where we find that has a value that is almost the same as for Data1.

We have used the range to fit a power law of the form given in eq. (1) to the measured after point source subtraction. The data points with error bars and the best fit power law are shown in Figure 3. Note that we have identified one of the Data1 points as an outlier and excluded it from the fit. The best fit parameters , the number of data points used for the fit and the chi-square per degree of freedom (reduced ) are listed in Table  1. The rather low values of the reduced indicate that the errors in the measured have possibly been somewhat overestimated. In order to validate our methodology we have simulated the visibility data for an input model power spectrum with the best fit values of the parameters and used this to estimate . The mean and errors (shaded region) estimated from realization of the simulation are shown in Figure 3. For the relevant range we find that the simulated is in very good agreement with the measured values thereby validating the entire fitting procedure. The horizontal lines in both the panels of Figure 3 show the predicted from the Poisson fluctuations of residual point sources below a threshold flux density of . The prediction here is based on the source counts of Ghosh et al. (2012). We find that for the measured values are well in excess of this prediction indicating that (1.) there are significant residual imaging artifacts around the bright source () which were subtracted , and/or (2.) the actual source distribution is in excess of the predictions of the source counts. Note that the actual values ( and for Data1 and Data2 respectively) are well below , and the corresponding predictions will lie below the horizontal lines shown in Figure 3.

For both the fields (Figure 3) is nearly flat at large and it is well modeled by a power law at smaller (). For Data1 the power law rises above the flat , and the power law is likely dominated by the DGSE. However, for Data2 the power law falls below the flat , and it is likely that in addition to the DGSE there is a significant residual point sources contribution. For Data2 we interpret the best fit power law as an upper limit for the DGSE.

The best fit parameters and for Data1 and Data2 respectively are compared with measurements from other observations such as Bernardi et al. (2009); Ghosh et al. (2012); Iacobelli et al. (2013) in Table 1. Further, we have also used an earlier work (La Porta et al. 2008) at higher frequencies and to estimate and compare the amplitude of the angular power spectrum of the DGSE expected at our observing frequency. Using the best-fit parameters (tabulated at = 100) at 408 and 1420 MHz, we extrapolate the amplitude of the at our observing frequency at for and . In this extrapolation we use a mean frequency spectral index of (de Oliveira-Costa et al. 2008) . The extrapolated amplitude values are shown in Table  1. In Table  1, we note that the angular power spectra of the DGSE in the northern hemisphere are comparatively larger than that of the southern hemisphere. The best fit parameter for Data1(Data2) agrees mostly with the extrapolated values obtained from () and ( ) within a factor of about 2 (4). The best fit parameter for Data1 and Data2 is within the range of 1.5-3.0 found by all the previous measurements at and higher frequencies.

The entire analysis here is based on the assumption that the DGSE is a Gaussian random field. This is possibly justified for the small patch of the sky under observation given that the diffuse emission is generated by a random processes like MHD turbulence. The estimated remains unaffected even if this assumption breaks down, only the error estimates will be changed. We note that the parameters are varying significantly from field to field across the different direction in the sky. We plan to extend this analysis for the whole sky and study the variation of the amplitude and power law index of using the full TGGS survey in future.

## 4 Acknowledgements

We thank an anonymous referee for helpful comments. S. Choudhuri would like to acknowledge the University Grant Commission, India for providing financial support. AG would like acknowledge Postdoctoral Fellowship from the South African Square Kilometre Array Project for financial support. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research.

## References

• Ali et al. (2008) Ali, S. S., Bharadwaj, S., & Chengalur, J. N. 2008, MNRAS, 385, 2166
• Bennett et al. (2003) Bennett C.L., Hill R.S., Hinshaw. G. et al., 2003, ApJS, 148, 97
• Bernardi et al. (2009) Bernardi, G., de Bruyn, A. G., Brentjens, M. A., et al. 2009, A & A, 500, 965
• Bharadwaj & Ali (2005) Bharadwaj, S., & Ali, S. S. 2005, MNRAS, 356, 1519
• Bowman et al. (2013) Bowman J. D. et al., 2013, PASA, 30, e031
• Choudhuri et al. (2014) Choudhuri, S., Bharadwaj, S., Ghosh, A., & Ali, S. S. 2014, MNRAS, 445, 4351
• Choudhuri et al. (2016) Choudhuri, S., Bharadwaj, S., Chatterjee, S., Ali, S. S., Roy, N., Ghosh, A., 2016, MNRAS, 463, 4093
• Choudhuri et al. (2016a) Choudhuri, S., Bharadwaj, S., Roy, N., Ghosh, A., & Ali, S. S., 2016a, MNRAS, 459, 151
• de Oliveira-Costa et al. (2008) de Oliveira-Costa A., Tegmark M., Gaensler B. M., Jonas J., Landecker T. L., Reich P., 2008, MNRAS, 388, 247
• Furlanetto et al. (2006) Furlanetto, S. R., Oh, S. P., & Briggs, F. H. 2006, Physics Reports, 433, 181
• Giardino et al. (2001) Giardino, G., Banday, A. J., Fosalba, P., et al. 2001, A & A, 371, 708
• Giardino et al. (2002) Giardino, G., Banday, A. J., Górski, K. M., et al. 2002, A & A, 387, 82
• Ghosh et al. (2011a) Ghosh, A., Bharadwaj, S., Ali, S. S., & Chengalur, J. N. 2011a, MNRAS, 411, 2426
• Ghosh et al. (2011b) Ghosh, A., Bharadwaj, S., Ali, S. S., & Chengalur, J. N. 2011b, MNRAS, 418, 2584
• Ghosh et al. (2012) Ghosh, A., Prasad, J., Bharadwaj, S., Ali, S. S., & Chengalur, J. N. 2012, MNRAS, 426, 3295
• Haslam et al. (1982) Haslam, C. G. T., Salter, C. J., Stoffel, H., & Wilson, W. E. 1982, A&AS  47, 1
• Iacobelli et al. (2013) Iacobelli, M., Haverkorn, M., Orrú, E., et al. 2013, A & A, 558, A72
• Intema et al. (2009) Intema, H. T., van der Tol, S., Cotton, W. D., et al. 2009, A & A, 501, 1185
• Intema (2014) Intema, H. T. 2014, arXiv:1402.4889
• Intema et al. (2016) Intema, H. T., Jagannathan, P., Mooley, K. P., & Frail, D. A. 2016, arXiv:1603.04368
• Koopmans et al. (2015) Koopmans, L., Pritchard, J., Mellema, G., et al. 2015, Advancing Astrophysics with the SKA (AASKA14), 1
• La Porta et al. (2008) La Porta, L., Burigana, C., Reich, W., & Reich, P. 2008, A & A, 479, 641
• Lazarian & Pogosyan (2012) Lazarian, A., & Pogosyan, D. 2012, ApJ, 747, 5
• Morales & Wyithe (2010) Morales, M. F., & Wyithe, J. S. B. 2010, ARAA, 48, 127
• Neben et al. (2016) Neben, A. R., Bradley, R. F., Hewitt, J. N., et al. 2016, ApJ, 826, 199
• Parsons et al. (2010) Parsons A. R. et al., 2010, AJ, 139, 1468
• Pritchard & Loeb (2012) Pritchard, J. R., & Loeb, A. 2012, Reports on Progress in Physics, 75, 086901
• Reich (1982) Reich, W. 1982, A&AS  48, 219
• Reich & Reich (1988) Reich, P., & Reich, W. 1988, A&AS, 74, 7
• Shaver et al. (1999) Shaver, P. A., Windhorst, R. A., Madau, P., & de Bruyn, A. G. 1999, A & A, 345, 380
• Sirothia et al. (2014) Sirothia, S. K., Lecavelier des Etangs, A., Gopal-Krishna, Kantharia, N. G., & Ishwar-Chandra, C. H. 2014, A & A, 562, A108
• Swarup et al. (1991) Swarup, G., Ananthakrishnan, S., Kapahi, V. K., Rao, A. P., Subrahmanya, C. R., and Kulkarni, V. K. 1991, CURRENT SCIENCE, 60, 95.
• var Haarlem et al. (2013) van Haarlem, M. P., Wise, M. W., Gunst, A. W., et al. 2013, A & A, 556, A2
• Waelkens et al. (2009) Waelkens, A. H., Schekochihin, A. A., & Enßlin, T. A. 2009, MNRAS, 398, 1970
You are adding the first comment!
How to quickly get a good reply:
• Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
• Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
• Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters