Pith. sign in

REVIEW 3 major objections 4 minor 96 references

GMRT observations of a first sample of Extremely Inverted Spectrum Extragalactic Radio Sources (EISERS) candidates in the Northern sky

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Quasi-simultaneous GMRT observations at 150 and 325 MHz claim two of fifteen candidate sources, J1326+5712 and J1658+4732, have spectral slopes +2.91 and +3.05, above the +2.5 SSA ceiling, confirming them as EISERS.

desk verdict Solid northern EISERS sample with one secure confirmation; the second object drops below threshold under the paper's own flux-scale correction. read the letter →

arxiv 1908.08883 v1 pith:NZKPHF7G submitted 2019-08-23 astro-ph.GA astro-ph.HE

Mukul Mhaskey , Gopal-Krishna , Surajit Paul , Pratik Dabhade , Sameer Salunkhe , Shubham Bhagat , Abhijit Bendre This is my paper · ORCID
classification astro-ph.GAastro-ph.HE
keywords extremelyinvertedspectrumradiosourcessynchrotronself-absorptionfree-freeabsorptionpeaked-spectrumGMRTobservationsTGSS-ADR1WENSSspectralindex
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper sets out to find extremely inverted spectrum extragalactic radio sources (EISERS) in the northern sky by taking fresh, quasi-simultaneous 150 and 325 MHz GMRT measurements of fifteen candidates shortlisted from the WENSS and TGSS-ADR1 surveys. The central claim is that two of these sources, J1326+5712 and J1658+4732, are bona fide EISERS, with two-point spectral slopes of $\alpha = +2.91 \pm 0.20$ and $+3.05 \pm 0.27$ across that band. That matters because the standard synchrotron self-absorption (SSA) explanation for inverted radio spectra, with a power-law electron population, cannot produce a slope steeper than $+2.5$ in the optically thick regime. If these slopes hold, the sharp turnovers must come from something else: a dense free-free absorbing screen of ionized gas, or a non-standard electron energy distribution. The paper also marks three candidates as possible EISERS and finds GPS-type spectra in nine of the fifteen sources.

What carries the argument

The load-bearing quantity is the two-point spectral index $\alpha$ computed between the uGMRT flux densities at 150 and 325 MHz, compared with the SSA critical value $\alpha_c = +2.5$, the optically thick slope $S_\nu \propto \nu^{5/2}$ that bounds a homogeneous incoherent synchrotron source with a power-law electron distribution. Because the underlying surveys were made a decade apart, the paper guards against calibration bias with field-based flux scaling factors (FSFs), ratios of bright in-field sources that rescale each 150 MHz uGMRT map to the TGSS-ADR1 flux scale. The interpretive machinery is the competition among four spectral models, SSA, homogeneous free-free absorption, internal free-free absorption, and the inhomogeneous free-free absorption of Bicknell et al., fitted to each source to decide which absorption process can produce the sharp turnover.

What would settle it

A single-epoch spectrum of J1658+4732 with narrowband coverage across 120-350 MHz on a flux scale tied directly to that source would settle it: if the 150-325 MHz slope stays above +2.5 with narrowband measurements, the FSF ambiguity becomes irrelevant; if it falls below +2.5, J1658+4732 loses its bona fide status.

Watch

Extended reading notes

Core claim

On its own measurements, the paper identifies J1326+5712 and J1658+4732 as confirmed EISERS. Their 150-325 MHz spectral indices, $\alpha = +2.91 \pm 0.20$ and $+3.05 \pm 0.27$, lie significantly above $\alpha_c = +2.5$, the hardness limit of the standard self-absorbed synchrotron spectrum $S_\nu \propto \nu^{5/2}$ for a homogeneous source. Both sources have GPS-like spectra peaking near 1 GHz, and their milliarcsecond structures are consistent with a compact symmetric object and a core-jet, respectively. Fitting four absorption models to the full spectra, the paper finds the inhomogeneous free-free absorption model of Bicknell et al. gives the best fit for both confirmed EISERS, with implied mean densities of the absorbing thermal gas of about 43 and 17 cm$^{-3}$ at the assumed velocity dispersion. Three more sources, J0847+5723, J0858+7501 and J1549+5038, are called possible EISERS because their slopes agree with $+2.5$ within 1$\sigma$.

Load-bearing premise

The claim that J1658+4732 is a bona fide EISERS assumes the field-based flux scaling factor that converts its uGMRT 150 MHz flux density to the TGSS-ADR1 scale is correct; with the paper's own FSF of 1.577 its spectral slope drops from +3.05 to +2.47, below the +2.5 threshold, and the FSF carries no quoted uncertainty.

Editorial extensions

If this is right

  • EISERS are extremely rare: only two of fifteen carefully selected candidates survive quasi-simultaneous measurement as bona fide cases, and the total known population remains a handful.
  • For both confirmed sources the inhomogeneous free-free absorption model is preferred, which would mean the ultra-sharp turnover comes from clumpy thermal gas surrounding the radio-emitting lobes rather than from the standard SSA mechanism.
  • The three possible EISERS are concrete follow-up targets: deeper, simultaneous metre-wavelength spectra could promote or remove each one.
  • Quasi-simultaneous observations are essential for this classification, since several candidates dropped out simply because their 150 MHz flux densities from decade-old surveys were unreliable, likely due to refractive interstellar scintillation.
  • If free-free absorption is confirmed, these sources probe dense ionized gas around young, parsec-scale radio sources; if not, they flag non-standard electron acceleration.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The status of J1658+4732 as bona fide EISERS is not settled on its own numbers: applying the paper's Table 4 flux scaling factor lowers its 150-325 MHz slope from $+3.05$ to $+2.47$, below the $+2.5$ threshold, and the FSF carries no quoted error.
  • A two-point slope says nothing about curvature; a single-epoch, multi-narrowband spectrum between 120 and 350 MHz for both confirmed sources would cleanly separate a power-law inverted slope from the curved signature of free-free absorption.
  • The candidate list was built from relatively bright sources in overlapping surveys, so the inferred rarity of EISERS is a lower limit; deeper overlapping surveys could reveal a fainter population with different physical conditions.
  • Spatially resolving the absorbing gas, through high-resolution imaging of the 150 MHz absorption against the VLBI core-jet, would test whether the free-free screen is external or internal to the synchrotron source.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper reports quasi-simultaneous uGMRT 150 MHz and 325 MHz observations of 15 extremely inverted spectrum radio source candidates selected from the overlap of TGSS-ADR1 and WENSS. Using the two measured flux densities, the authors compute spectral indices in the optically thick part of the spectrum and identify two 'bona fide' EISERS (J1326+5712 and J1658+4732) with slopes of +2.91±0.20 and +3.05±0.27, above the SSA critical value +2.5; three further sources are close to the threshold and are called tentative. The paper also fits SSA and free-free absorption spectral models to the sources, derives physical parameters (absorbing gas densities, magnetic fields) for selected sources, and summarizes VLBI structural information. A flux scaling factor (FSF) calibration is applied to check the 150 MHz uGMRT flux scale against TGSS-ADR1; Table 4 lists FSF values and the resulting adjusted spectral indices.

Significance. If both headline objects are genuine, the sample would add to the very small list of known EISERS and would strengthen the case that some compact radio sources exhibit a turnover steeper than the canonical SSA limit, motivating non-standard electron energy distributions or widespread free-free absorption. The paper's strengths include the quasi-simultaneous two-frequency uGMRT observations, a well-documented survey-based selection procedure, comparison of SSA and FFA model families, and VLBI context for individual sources. The central classification is a threshold test, however, and its reliability depends on calibration systematics that are not fully quantified; the most serious issue is the effect of the FSF correction on J1658+4732, which, by the paper's own numbers, drops the central spectral index to 2.47, below the threshold.

major comments (3)
  1. [Section 6 and Table 4] The statement in Section 6 that 'the spectral indices of the two confirmed EISERS would remain above the SSA limit ... even if their present flux densities measured at 150 MHz with uGMRT are aligned with the flux scale of the TGSS-ADR1' is contradicted by the paper's own Table 4 for J1658+4732. Applying FSF = 1.577 to the uGMRT 150 MHz flux density of 15.4±2.8 mJy gives a rescaled 150 MHz flux density of about 24.3 mJy, and the quoted 325 MHz uGMRT flux density of 163.4±16.4 mJy yields alpha(150-325 MHz) = 2.47±0.32, which lies below alpha_c = +2.5. Only J1326+5712 remains above the threshold after the FSF correction (alpha = 3.24±0.20). The sentence in Section 6 is therefore internally inconsistent with Table 4, and the 'two bona fide EISERS' claim appears to be one object short unless J1658+4732 is re-evaluated with a full treatment of calibration uncertainty.
  2. [Section 3.2 and Table 4] The FSF values in Table 4 are quoted as single numbers without uncertainties, and this omission is load-bearing because the EISERS classification is a threshold test. For J1658+4732 the threshold alpha_c = +2.5 is crossed when FSF is about 1.535, only about 3% below the adopted 1.577, while the FSF values span 0.390-1.577 across the fifteen fields and are derived from only a few bright comparison sources per field. A calibration error of a few percent, much smaller than the 10% systematic error included in Eq. (1), would move J1658+4732 across the boundary. The authors should quote the FSF uncertainties (e.g., the RMS scatter about the mean ratio and the number of comparison sources used in each field) and propagate them into the threshold test before labeling J1658+4732 a bona fide EISERS.
  3. [Section 3.2 and Table 4] The FSF correction as implemented rescales only the 150 MHz uGMRT flux densities to the TGSS-ADR1 scale; the 325 MHz uGMRT flux densities are not independently tied to an absolute flux scale. This matters because Section 3 notes that WENSS deviates from the RCB/Baars flux scales by more than 10%, and Section 4 documents differences of roughly 20-25% between some uGMRT 325 MHz measurements and the WENSS values (e.g., J1326+5712 is about 75% of the WENSS value, and J1846+4239 differs substantially). A 10% scale error at 325 MHz changes alpha(150-325) by about 0.3 in this frequency ratio, which is comparable to the quoted 1-sigma uncertainties and to the margin separating J1658+4732 from alpha_c. The threshold test should include a corresponding check of the 325 MHz scale, for example against WENSS or a calibrator-based measurement, before the two-object conclusion is presented as secure.
minor comments (4)
  1. [Section 3.1] The text refers to 'J1658+473' in the sentence about Figures 1 and 2; this should be 'J1658+4732'.
  2. [Section 5.4] The phrase 'For the confirmed EISERS where in-homogeneous FFA model ... namely, J0847+5723, J1326+5712 and J1658+4732' is inaccurate because J0847+5723 is classified as 'Tentative' rather than 'Bona fide' in Table 3; please rephrase to 'for the sources where the inhomogeneous FFA model provides the best fit'.
  3. [Section 6] In the discussion of the Callingham et al. (2017) sources, the same name 'J213024-434819' appears twice; the second instance should presumably be a different source name and should be corrected.
  4. [Section 6] The sentence 'The radio power at 5 GHz are presentented in Table 3' contains a typo: 'presentented' should be 'presented'.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: EISERS confirmation uses new uGMRT flux densities against an externally established SSA limit; the Table 4/Section 6 FSF tension is a calibration robustness issue, not a circular derivation.

full rationale

The paper's central claim is a measured two-point spectral index from new uGMRT observations compared against the externally established SSA limit alpha_c = +2.5 (Slish 1963; Scheuer & Williams 1968; Rybicki & Lightman 1986), not against a quantity fitted from the same data. The candidate list was selected from TGSS/WENSS catalogue flux densities, while the confirmation uses independent quasi-simultaneous uGMRT flux densities, so the confirmation is not forced by the selection. The FSF rescaling in Section 3.2 is calibrated using unrelated bright sources within each field; it is not fitted to the target's 150-325 MHz slope, so the adjusted indices are a cautionary recalibration rather than a fitted prediction. Self-citations to Papers I and II establish the class name and earlier candidate lists, but the SSA limit itself is supported by independent classical references. There is a real internal tension: for J1658+4732, applying FSF = 1.577 gives alpha_TGSS = 2.47 +/- 0.32 (Table 4), below alpha_c = 2.5, while Section 6 asserts both confirmed EISERS 'would remain above the SSA limit' even after rescaling; the FSF values also carry no quoted uncertainties, and the paper explicitly notes the small number of fields 'does not allow us to make a general comment about the origin of the occasionally significant departures of FSF values from unity.' This is a calibration robustness/correctness problem, not circularity, because the classification rests on directly measured flux densities and an external threshold. No derivation step reduces to its own input or to an unverified self-citation, so the circularity score is 0.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central classification rests on two-point spectral indices measured from new uGMRT observations. The only fitted quantities are the parameters of the absorption model SED fits (normalizations, turnover frequencies, intrinsic spectral indices, and the inhomogeneity index p), which do not feed back into the EISERS classification. The main structural assumptions are the external SSA limit, the reliability of the flux-density scales, and assumed redshifts and velocity dispersions for physical parameter estimates.

free parameters (4)
  • Normalization amplitude a_i (SSA and FFA models) = Not reported
    Each absorption model in Eqs. 3, 5, 6, 7 has a free normalization fitted to the observed spectrum; best-fit values are not tabulated.
  • Turnover frequency nu_p = Reported per source in Table 5 (e.g., 0.73 GHz for J1326+5712)
    The frequency at which optical depth is unity is a fitted parameter for each model, and the best-fit peak frequency is listed in Table 5.
  • Intrinsic spectral index alpha (FFA models) = Not reported
    In the FFA models (Eqs. 5-7), the intrinsic optically thin spectral index alpha is fitted along with the normalization and turnover frequency.
  • Inhomogeneity index p (Bicknell et al. 1997 model) = Not reported
    The power-law index of the free-free optical depth distribution in Eq. 7 is fitted per source; the best-fit values are not given.
assumptions (5)
  • domain assumption Standard SSA limit: a homogeneous, incoherent synchrotron source with a power-law electron energy distribution cannot produce a low-frequency spectral slope steeper than alpha_c = +2.5.
    Used in Section 1 and Section 5.1 to define the EISERS threshold; from Slish 1963 and Scheuer & Williams 1968.
  • domain assumption The two-point spectral index between 150 and 325 MHz measured from quasi-simultaneous uGMRT observations is a reliable estimate of the optically thick spectral slope, unaffected by variability or resolution effects.
    Used throughout; mitigated by quasi-simultaneity (Section 6) but still assumes the sources are compact and not resolved out at either frequency.
  • ad hoc to paper The flux-density scale of the uGMRT 150 MHz maps can be corrected to the TGSS-ADR1 scale using field-based FSF values computed from other bright sources.
    Introduced in Section 3.2 and Table 4; no uncertainties on FSF, and FSF varies from 0.39 to 1.58, indicating large systematic offsets.
  • domain assumption For sources without redshifts, z=1 is assumed when computing 5 GHz radio powers.
    Stated in Section 2 and Table 3 footnote; affects the radio power estimates but not the EISERS classification.
  • domain assumption The absorbing medium in the FFA interpretation is assumed to have a baryonic velocity dispersion of 250 km/s.
    Assumed in Section 5.4 following Forster Schreiber et al. (2009) and Mukherjee et al. (2016); used to convert fitted parameters to mean densities.

how reviews work

0 comments
Cite this review

Pith. "Pith review of GMRT observations of a first sample of Extremely Inverted Spectrum Extragalactic Radio Sources (EISERS) candidates in the Northern sky." pith.science (2026). https://pith.science/paper/NZKPHF7G

@misc{pith2026190808883,
  author       = {Pith},
  title        = {Pith review of: GMRT observations of a first sample of Extremely Inverted Spectrum Extragalactic Radio Sources (EISERS) candidates in the Northern sky},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NZKPHF7G}},
  note         = {Machine review of arXiv:1908.08883}
}
abstract

We present an extension of our search for Extremely Inverted Spectrum Extragalactic Radio Sources (EISERS) to the northern celestial hemisphere. With an inverted radio spectrum of slope $\alpha$ > +2.5, these rare sources would either require a non-standard particle acceleration mechanism (in the framework of synchrotron self-absorption hypothesis), or a severe free-free absorption which attenuates practically all of their synchrotron radiation at metre wavelengths. By applying a sequence of selection filters, a list of 15 EISERS candidates is extracted out by comparing two large-sky radio surveys, WENSS (325 MHz) and TGSS-ADR1 (150 MHz), which overlap across 1.03$\pi$ steradian of the sky. Here we report quasi-simultaneous GMRT observations of these 15 EISERS candidates at 150 MHz and 325 MHz, in an attempt to accurately define their spectra below the turnover frequency. Out of the 15 candidates observed, two are confirmed as EISERS, since the slope of the inverted spectrum between these two frequencies is found to be significantly larger than the critical value $\alpha_c$ = +2.5: the theoretical limit for the standard case of synchrotron self-absorption (SSA). For another 3 sources, the spectral slope is close to, or just above the critical value $\alpha_c$. Nine of the sources have GPS type radio spectra. The parsec-scale radio structural information available for the sample is also summarised.

Figures

Figures reproduced from arXiv: 1908.08883 by the authors.

Figure 1
Figure 1. The uGMRT contour maps of J1326+5712 at 150 MHz and 325 MHz, respectively. The contours are drawn at 3, 4, 8, 16, 32, 64 and 128 times the image rms noise which is 1.2 mJy at 150 MHz and 0.5 mJy at 325 MHz. The FWHMs are 26 × 18” (PA= 9◦) and 12 × 7” (PA= −10◦) at 150 MHz and 325 MHz, respectively. The target source lies at the centre of each map [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 3
Figure 3. Radio spectra of the 15 EISERS candidates (see [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Different absorption models fitted to the spectral energy distributions of the bonafide EISERS J1326+5712 and J1658+4732. In both cases the inhomogeneous FFA model provides the best fit (see Section5). 6 DISCUSSION From [PITH_FULL_IMAGE:figures/full_fig_p012_4.png] view at source ↗
Figures from the paper (8 more)
Figure 1
Figure 1. Figure 1: GMRT contour maps of J0045+8810 at 150 MHz and 325 MHz, respectively. The contour levels are 3,4,8,16,32,64 & 128 with the unit contour level at 150 MHz at 3.5 mJy and 1.0 mJy at 325 MHz. The beam size is 24 × 15” (PA= 53◦) and 25 × 06” (PA= 69◦) at 150 MHz and 325 MHz…
Figure 3
Figure 3. Figure 3: GMRT contour maps of J0754+5324 at 150 MHz and 325 MHz, respectively. The contour levels are 3,4,8,16,32,64 & 128 with the unit contour level at 150 MHz at 3.8 mJy and 0.6 mJy at 325 MHz. The beam size is 55 × 13” (PA= −87◦) and 15 × 07” (PA= 70◦) at 150 MHz and 325 MH…
Figure 5
Figure 5. Figure 5: GMRT contour maps of J0858+7501 at 150 MHz and 325 MHz, respectively. The contour levels are 3,4,8,16,32,64 & 128 with the unit contour level at 150 MHz at 3.8 mJy and 0.7 mJy at 325 MHz. The beam size is 47 × 14” (PA= 85◦) and 22 × 06” (PA= 84◦) at 150 MHz and 325 MHz…
Figure 8
Figure 8. Figure 8: GMRT contour maps of J1549+5038 at 150 MHz and 325 MHz, respectively. The contour levels are 3,4,8,16,32,64 & 128 with the unit contour level at 150 MHz at 1.5 mJy and 0.6 mJy at 325 MHz. The beam size is 24 × 19” (PA= 09◦) and 11 × 07” (PA= 04◦) at 150 MHz and 325 MHz…
Figure 9
Figure 9. Figure 9: GMRT contour maps of J1700+3830 at 150 MHz and 325 MHz, respectively. The contour levels are 3,4,8,16,32,64 & 128 with the unit contour level at 150 MHz at 2.5 mJy and 0.5 mJy at 325 MHz. The beam size is 20 × 14” (PA= 26◦) and 09 × 07” (PA= −12◦) at 150 MHz and 325 MH…
Figure 11
Figure 11. Figure 11: GMRT contour maps of J1723+7653 at 150 MHz and 325 MHz, respectively. The contour levels are 3,4,8,16,32,64 & 128 with the unit contour level at 150 MHz at 2.0 mJy and 1.0 mJy at 325 MHz. The beam size is 34 × 16” (PA= 08◦) and 17 × 07” (PA= 30◦) at 150 MHz and 325 MH…
Figure 13
Figure 13. Figure 13: GMRT contour maps of J2317+4738 at 150 MHz and 325 MHz, respectively. The contour levels are 3,4,8,16,32,64 & 128 with the unit contour level at 150 MHz at 2.5 mJy and 0.8 mJy at 325 MHz. The beam size is 21 × 20” (PA= 23◦) and 13 × 08” (PA= −62◦) at 150 MHz and 325 M…
Figure 14
Figure 14. Figure 14: Different absorption models fitted to the spectral energy distribution of the observed EISERS candidates. 8 [PITH_FULL_IMAGE:figures/full_fig_p026_14.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

96 extracted references · 24 canonical work pages

  1. [1]

    Alam S., et al., 2015, @doi [ ] 10.1088/0067-0049/219/1/12 , http://adsabs.harvard.edu/abs/2015ApJS..219...12A 219, 12

    doi:10.1088/0067-0049/219/1/12 2015

  2. [2]

    A., 2012, @doi [ ] 10.1088/0004-637X/760/1/77 , http://adsabs.harvard.edu/abs/2012ApJ...760...77A 760, 77

    An T., Baan W. A., 2012, @doi [ ] 10.1088/0004-637X/760/1/77 , http://adsabs.harvard.edu/abs/2012ApJ...760...77A 760, 77

    doi:10.1088/0004-637x/760/1/77 2012

  3. [3]

    Asano K., Takahara F., Kusunose M., Toma K., Kakuwa J., 2014, @doi [ ] 10.1088/0004-637X/780/1/64 , https://ui.adsabs.harvard.edu/abs/2014ApJ...780...64A 780, 64

    doi:10.1088/0004-637x/780/1/64 2014

  4. [4]

    Baars J. W. M., Genzel R., Pauliny-Toth I. I. K., Witzel A., 1977, , http://adsabs.harvard.edu/abs/1977A

    1977

  5. [5]

    D., Capetti A., Giovannini G., 2015, @doi [ ] 10.1051/0004-6361/201425426 , http://adsabs.harvard.edu/abs/2015A

    Baldi R. D., Capetti A., Giovannini G., 2015, @doi [ ] 10.1051/0004-6361/201425426 , http://adsabs.harvard.edu/abs/2015A

    doi:10.1051/0004-6361/201425426 2015

  6. [6]

    C., 1996, Baby Cygnus A's

    Begelman M. C., 1996, Baby Cygnus A's . p. 209

    1996

  7. [7]

    E., et al., 2019, @doi [ ] 10.1093/mnras/sty2801 , http://adsabs.harvard.edu/abs/2019MNRAS.482.2484B 482, 2484

    Bell M. E., et al., 2019, @doi [ ] 10.1093/mnras/sty2801 , http://adsabs.harvard.edu/abs/2019MNRAS.482.2484B 482, 2484

    doi:10.1093/mnras/sty2801 2019

  8. [8]

    N., Kauffmann G., Heckman T

    Best P. N., Kauffmann G., Heckman T. M., Ivezi \'c Z ., 2005, @doi [ ] 10.1111/j.1365-2966.2005.09283.x , http://adsabs.harvard.edu/abs/2005MNRAS.362....9B 362, 9

    arXiv 2005

Show all 96 references
  1. [9]

    V., Dopita M

    Bicknell G. V., Dopita M. A., O'Dea C. P. O., 1997, @doi [ ] 10.1086/304400 , http://adsabs.harvard.edu/abs/1997ApJ...485..112B 485, 112

    1997 doi

  2. [10]

    V., Mukherjee D., Wagner A

    Bicknell G. V., Mukherjee D., Wagner A. Y., Sutherland R. S., Nesvadba N. P. H., 2018, @doi [ ] 10.1093/mnras/sty070 , http://adsabs.harvard.edu/abs/2018MNRAS.475.3493B 475, 3493

    2018 doi

  3. [11]

    R., et al., 2015, @doi [ ] 10.1088/0004-637X/809/2/168 , http://adsabs.harvard.edu/abs/2015ApJ...809..168C 809, 168

    Callingham J. R., et al., 2015, @doi [ ] 10.1088/0004-637X/809/2/168 , http://adsabs.harvard.edu/abs/2015ApJ...809..168C 809, 168

    2015 doi

  4. [12]

    R., et al., 2017, @doi [ ] 10.3847/1538-4357/836/2/174 , http://adsabs.harvard.edu/abs/2017ApJ...836..174C 836, 174

    Callingham J. R., et al., 2017, @doi [ ] 10.3847/1538-4357/836/2/174 , http://adsabs.harvard.edu/abs/2017ApJ...836..174C 836, 174

    2017 doi

  5. [13]

    Chandra P., Ray A., Bhatnagar S., 2004, @doi [ ] 10.1086/422675 , http://adsabs.harvard.edu/abs/2004ApJ...612..974C 612, 974

    2004 doi

  6. [14]

    Cheung E., et al., 2013, @doi [ ] 10.1088/0004-637X/779/2/162 , http://adsabs.harvard.edu/abs/2013ApJ...779..162C 779, 162

    2013 doi

  7. [15]

    J., Cotton W

    Condon J. J., Cotton W. D., Greisen E. W., Yin Q. F., Perley R. A., Taylor G. B., Broderick J. J., 1998, @doi [ ] 10.1086/300337 , http://adsabs.harvard.edu/abs/1998AJ....115.1693C 115, 1693

    1998 doi

  8. [16]

    E., Myers S

    Conway J. E., Myers S. T., Pearson T. J., Readhead A. C. S., Unwin S. C., Xu W., 1994, @doi [ ] 10.1086/174006 , http://adsabs.harvard.edu/abs/1994ApJ...425..568C 425, 568

    1994 doi

  9. [17]

    P., Ortega-Minakata R

    Coziol R., Andernach H., Torres-Papaqui J. P., Ortega-Minakata R. A., Moreno del Rio F., 2017, @doi [ ] 10.1093/mnras/stw3164 , http://adsabs.harvard.edu/abs/2017MNRAS.466..921C 466, 921

    2017 doi

  10. [18]

    Dabhade P., Gaikwad M., Bagchi J., Pandey-Pommier M., Sankhyayan S., Raychaudhury S., 2017, @doi [ ] 10.1093/mnras/stx860 , http://adsabs.harvard.edu/abs/2017MNRAS.469.2886D 469, 2886

    2017 doi

  11. [19]

    Dallacasa D., Stanghellini C., Centonza M., Fanti R., 2000, , http://adsabs.harvard.edu/abs/2000A

    2000

  12. [20]

    G., R \"o ttgering H., van Breugel W., 2002, @doi [ ] 10.1051/0004-6361:20021115 , http://adsabs.harvard.edu/abs/2002A

    De Breuck C., Tang Y., de Bruyn A. G., R \"o ttgering H., van Breugel W., 2002, @doi [ ] 10.1051/0004-6361:20021115 , http://adsabs.harvard.edu/abs/2002A

    2002 doi

  13. [21]

    N., Bash F

    Douglas J. N., Bash F. N., Bozyan F. A., Torrence G. W., Wolfe C., 1996, @doi [ ] 10.1086/117932 , http://adsabs.harvard.edu/abs/1996AJ....111.1945D 111, 1945

    1996 doi

  14. [22]

    L., Charlot P., 2000, @doi [ ] 10.1086/313382 , http://adsabs.harvard.edu/abs/2000ApJS..128...17F 128, 17

    Fey A. L., Charlot P., 2000, @doi [ ] 10.1086/313382 , http://adsabs.harvard.edu/abs/2000ApJS..128...17F 128, 17

    2000 doi

  15. [23]

    M., et al., 2009, @doi [ ] 10.1088/0004-637X/706/2/1364 , https://ui.adsabs.harvard.edu/abs/2009ApJ...706.1364F 706, 1364

    F \"o rster Schreiber N. M., et al., 2009, @doi [ ] 10.1088/0004-637X/706/2/1364 , https://ui.adsabs.harvard.edu/abs/2009ApJ...706.1364F 706, 1364

    2009 doi

  16. [24]

    Gopal-Krishna Spoelstra T. A. T., 1993, , http://adsabs.harvard.edu/abs/1993A

    1993

  17. [25]

    J., 2000, , http://adsabs.harvard.edu/abs/2000A

    Gopal-Krishna Wiita P. J., 2000, , http://adsabs.harvard.edu/abs/2000A

    2000

  18. [26]

    R., Steppe H., 1983, , http://adsabs.harvard.edu/abs/1983A

    Gopal-Krishna Patnaik A. R., Steppe H., 1983, , http://adsabs.harvard.edu/abs/1983A

    1983

  19. [27]

    L., Gergely L

    Gopal-Krishna Biermann P. L., Gergely L. \'A ., Wiita P. J., 2012, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/12/2/002 , http://adsabs.harvard.edu/abs/2012RAA....12..127G 12, 127

    2012 doi

  20. [28]

    K., Mhaskey M., Ranadive P., Wiita P

    Gopal-Krishna Sirothia S. K., Mhaskey M., Ranadive P., Wiita P. J., Goyal A., Kantharia N. G., Ishwara-Chandra C. H., 2014, @doi [ ] 10.1093/mnras/stu1364 , http://adsabs.harvard.edu/abs/2014MNRAS.443.2824K 443, 2824

    2014 doi

  21. [29]

    C., Condon J

    Gregory P. C., Condon J. J., 1991, @doi [ ] 10.1086/191559 , http://adsabs.harvard.edu/abs/1991ApJS...75.1011G 75, 1011

    1991 doi

  22. [30]

    E., Taylor G

    Gugliucci N. E., Taylor G. B., Peck A. B., Giroletti M., 2005, @doi [ ] 10.1086/427934 , http://adsabs.harvard.edu/abs/2005ApJ...622..136G 622, 136

    2005 doi

  23. [31]

    Gupta Y., et al., 2017, Current Science, 113, 707

    2017

  24. [32]

    Hales S. E. G., Mayer C. J., Warner P. J., Baldwin J. E., 1991, @doi [ ] 10.1093/mnras/251.1.46 , https://ui.adsabs.harvard.edu/abs/1991MNRAS.251...46H 251, 46

    1991 doi

  25. [33]

    J., et al., 2016, @doi [ ] 10.1093/mnras/stw1763 , http://adsabs.harvard.edu/abs/2016MNRAS.462.1910H 462, 1910

    Hardcastle M. J., et al., 2016, @doi [ ] 10.1093/mnras/stw1763 , http://adsabs.harvard.edu/abs/2016MNRAS.462.1910H 462, 1910

    2016 doi

  26. [34]

    J., White R

    Helfand D. J., White R. L., Becker R. H., 2015, @doi [ ] 10.1088/0004-637X/801/1/26 , http://adsabs.harvard.edu/abs/2015ApJ...801...26H 801, 26

    2015 doi

  27. [35]

    F., et al., 2007, @doi [ ] 10.1086/511005 , http://adsabs.harvard.edu/abs/2007ApJ...658..203H 658, 203

    Helmboldt J. F., et al., 2007, @doi [ ] 10.1086/511005 , http://adsabs.harvard.edu/abs/2007ApJ...658..203H 658, 203

    2007 doi

  28. [36]

    Hurley-Walker N., et al., 2017, @doi [ ] 10.1093/mnras/stw2337 , http://adsabs.harvard.edu/abs/2017MNRAS.464.1146H 464, 1146

    2017 doi

  29. [37]

    T., 2014, in Astronomical Society of India Conference Series

    Intema H. T., 2014, in Astronomical Society of India Conference Series. ( @eprint arXiv 1402.4889 )

    2014 arXiv

  30. [38]

    T., Jagannathan P., Mooley K

    Intema H. T., Jagannathan P., Mooley K. P., Frail D. A., 2017, @doi [ ] 10.1051/0004-6361/201628536 , http://adsabs.harvard.edu/abs/2017A

    2017 doi

  31. [39]

    Jauncey D., et al., 2016, @doi [Galaxies] 10.3390/galaxies4040062 , http://adsabs.harvard.edu/abs/2016Galax...4...62J 4, 62

    2016 doi

  32. [40]

    L., et al., 1996, @doi [ ] 10.1086/310183 , http://adsabs.harvard.edu/abs/1996ApJ...466L..63J 466, L63

    Jones D. L., et al., 1996, @doi [ ] 10.1086/310183 , http://adsabs.harvard.edu/abs/1996ApJ...466L..63J 466, L63

    1996 doi

  33. [41]

    Kameno S., Horiuchi S., Shen Z.-Q., Inoue M., Kobayashi H., Hirabayashi H., Murata Y., 2000, @doi [ ] 10.1093/pasj/52.1.209 , http://adsabs.harvard.edu/abs/2000PASJ...52..209K 52, 209

    2000 doi

  34. [42]

    D., et al., 2017, @doi [ ] 10.3847/1538-3881/aa90b7 , http://adsabs.harvard.edu/abs/2017AJ....154..253K 154, 253

    Kapi \'n ska A. D., et al., 2017, @doi [ ] 10.3847/1538-3881/aa90b7 , http://adsabs.harvard.edu/abs/2017AJ....154..253K 154, 253

    2017 doi

  35. [43]

    I., 1966, @doi [Australian Journal of Physics] 10.1071/PH660195 , http://adsabs.harvard.edu/abs/1966AuJPh..19..195K 19, 195

    Kellermann K. I., 1966, @doi [Australian Journal of Physics] 10.1071/PH660195 , http://adsabs.harvard.edu/abs/1966AuJPh..19..195K 19, 195

    1966 doi

  36. [44]

    I., Pauliny-Toth I

    Kellermann K. I., Pauliny-Toth I. I. K., 1969, @doi [ ] 10.1086/180305 , http://adsabs.harvard.edu/abs/1969ApJ...155L..71K 155, L71

    1969 doi

  37. [45]

    P., Alef W., Witzel A., Zensus J

    Krichbaum T. P., Alef W., Witzel A., Zensus J. A., Booth R. S., Greve A., Rogers A. E. E., 1998, , http://adsabs.harvard.edu/abs/1998A

    1998

  38. [46]

    V., Dopita M

    Kuncic Z., Bicknell G. V., Dopita M. A., 1998, @doi [ ] 10.1086/311202 , http://adsabs.harvard.edu/abs/1998ApJ...495L..35K 495, L35

    1998 doi

  39. [47]

    Ku \'z micz A., Jamrozy M., Kozie -Wierzbowska D., We \.z gowiec M., 2017, @doi [ ] 10.1093/mnras/stx1830 , http://adsabs.harvard.edu/abs/2017MNRAS.471.3806K 471, 3806

    2017 doi

  40. [48]

    M., Cotton W

    Lane W. M., Cotton W. D., van Velzen S., Clarke T. E., Kassim N. E., Helmboldt J. F., Lazio T. J. W., Cohen A. S., 2014, @doi [ ] 10.1093/mnras/stu256 , http://adsabs.harvard.edu/abs/2014MNRAS.440..327L 440, 327

    2014 doi

  41. [49]

    Lazio T. J. W., Cordes J. M., de Bruyn A. G., Macquart J.-P., 2004, @doi [ ] 10.1016/j.newar.2004.09.039 , http://adsabs.harvard.edu/abs/2004NewAR..48.1439L 48, 1439

    2004 doi

  42. [50]

    C., 1995, @doi [ ] 10.1086/175988 , http://adsabs.harvard.edu/abs/1995ApJ...448..589L 448, 589

    Levinson A., Laor A., Vermeulen R. C., 1995, @doi [ ] 10.1086/175988 , http://adsabs.harvard.edu/abs/1995ApJ...448..589L 448, 589

    1995 doi

  43. [51]

    R., Gawro \'n ski M

    Lowe S. R., Gawro \'n ski M. P., Wilkinson P. N., Kus A. J., Browne I. W. A., Pazderski E., Feiler R., Kettle D., 2007, @doi [ ] 10.1051/0004-6361:20078034 , http://adsabs.harvard.edu/abs/2007A

    2007 doi

  44. [52]

    I., Pauliny-Toth I

    Matveenko L. I., Pauliny-Toth I. I. K., Sherwood W., 1990, Soviet Astronomy Letters, http://adsabs.harvard.edu/abs/1990SvAL...16..247M 16, 247

    1990

  45. [53]

    K., 2019, @doi [ ] 10.1093/mnras/stz335 , http://adsabs.harvard.edu/abs/2019MNRAS.tmp..341M

    Mhaskey M., Gopal-Krishna Pratik D., Paul S., Salunkhe S., Sirothia S. K., 2019, @doi [ ] 10.1093/mnras/stz335 , http://adsabs.harvard.edu/abs/2019MNRAS.tmp..341M

    2019 doi

  46. [54]

    V., Sutherland R., Wagner A., 2016, @doi [ ] 10.1093/mnras/stw1368 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461..967M 461, 967

    Mukherjee D., Bicknell G. V., Sutherland R., Wagner A., 2016, @doi [ ] 10.1093/mnras/stw1368 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461..967M 461, 967

    2016 doi

  47. [55]

    T., et al., 2003, VizieR Online Data Catalog, http://adsabs.harvard.edu/abs/2003yCat.8072....0M 8072

    Myers S. T., et al., 2003, VizieR Online Data Catalog, http://adsabs.harvard.edu/abs/2003yCat.8072....0M 8072

    2003

  48. [56]

    P., 1998, @doi [ ] 10.1086/316162 , http://adsabs.harvard.edu/abs/1998PASP..110..493O 110, 493

    O'Dea C. P., 1998, @doi [ ] 10.1086/316162 , http://adsabs.harvard.edu/abs/1998PASP..110..493O 110, 493

    1998 doi

  49. [57]

    Orienti M., Dallacasa D., 2008, @doi [ ] 10.1051/0004-6361:20078098 , http://adsabs.harvard.edu/abs/2008A

    2008 doi

  50. [58]

    Orienti M., Dallacasa D., Stanghellini C., 2007, @doi [ ] 10.1051/0004-6361:20078105 , https://ui.adsabs.harvard.edu/abs/2007A&A...475..813O 475, 813

    2007 doi

  51. [59]

    G., 1970, Radio astrophysics

    Pacholczyk A. G., 1970, Radio astrophysics. Nonthermal processes in galactic and extragalactic sources

    1970

  52. [60]

    P \^a ris I., et al., 2017, @doi [ ] 10.1051/0004-6361/201527999 , http://adsabs.harvard.edu/abs/2017A

    2017 doi

  53. [61]

    Pasetto A., Kraus A., Mack K.-H., Bruni G., Carrasco-Gonz \'a lez C., 2016, @doi [ ] 10.1051/0004-6361/201526963 , http://adsabs.harvard.edu/abs/2016A

    2016 doi

  54. [62]

    B., Taylor G

    Peck A. B., Taylor G. B., 2000, @doi [ ] 10.1086/308746 , http://adsabs.harvard.edu/abs/2000ApJ...534...90P 534, 90

    2000 doi

  55. [63]

    B., Mutel R

    Phillips R. B., Mutel R. L., 1982, , http://adsabs.harvard.edu/abs/1982A

    1982

  56. [64]

    J., 1967, @doi [ ] 10.1093/mnras/136.3.279 , http://adsabs.harvard.edu/abs/1967MNRAS.136..279R 136, 279

    Rees M. J., 1967, @doi [ ] 10.1093/mnras/136.3.279 , http://adsabs.harvard.edu/abs/1967MNRAS.136..279R 136, 279

    1967 doi

  57. [65]

    B., Tang Y., de Bruyn A

    Rengelink R. B., Tang Y., de Bruyn A. G., Miley G. K., Bremer M. N., Roettgering H. J. A., Bremer M. A. R., 1997, @doi [ ] 10.1051/aas:1997358 , http://adsabs.harvard.edu/abs/1997A

    1997 doi

  58. [66]

    L., et al., 2011, @doi [ ] 10.1088/0067-0049/194/2/29 , http://adsabs.harvard.edu/abs/2011ApJS..194...29R 194, 29

    Richards J. L., et al., 2011, @doi [ ] 10.1088/0067-0049/194/2/29 , http://adsabs.harvard.edu/abs/2011ApJS..194...29R 194, 29

    2011 doi

  59. [67]

    L., Hovatta T., Max-Moerbeck W., Pavlidou V., Pearson T

    Richards J. L., Hovatta T., Max-Moerbeck W., Pavlidou V., Pearson T. J., Readhead A. C. S., 2014, @doi [ ] 10.1093/mnras/stt2412 , http://adsabs.harvard.edu/abs/2014MNRAS.438.3058R 438, 3058

    2014 doi

  60. [68]

    J., Coles W

    Rickett B. J., Coles W. A., Bourgois G., 1984, , http://adsabs.harvard.edu/abs/1984A

    1984

  61. [69]

    H., Saripalli L., Wang K

    Roberts D. H., Saripalli L., Wang K. X., Sathyanarayana Rao M., Subrahmanyan R., KleinStern C. C., Morii-Sciolla C. Y., Simpson L., 2018, @doi [ ] 10.3847/1538-4357/aa9c49 , http://adsabs.harvard.edu/abs/2018ApJ...852...47R 852, 47

    2018 doi

  62. [70]

    S., Costain C

    Roger R. S., Costain C. H., Bridle A. H., 1973, @doi [ ] 10.1086/111506 , http://adsabs.harvard.edu/abs/1973AJ.....78.1030R 78, 1030

    1973 doi

  63. [71]

    B., Lightman A

    Rybicki G. B., Lightman A. P., 1986, Radiative Processes in Astrophysics

    1986

  64. [72]

    Scheuer P. A. G., Williams P. J. S., 1968, @doi [ ] 10.1146/annurev.aa.06.090168.001541 , http://adsabs.harvard.edu/abs/1968ARA

    1968

  65. [73]

    pp 355--360

    Schlickeiser R., 1985, Particle acceleration in active galactic nuclei - coexistence of monoenergetic, power law and Maxwell-Boltzmann electron energy spectra. . pp 355--360

    1985

  66. [74]

    Y., 1978, , http://adsabs.harvard.edu/abs/1978SvA....22..544S 22, 544

    Shapirovskaya N. Y., 1978, , http://adsabs.harvard.edu/abs/1978SvA....22..544S 22, 544

    1978

  67. [75]

    W., et al., 2017, @doi [ ] 10.1051/0004-6361/201629313 , http://adsabs.harvard.edu/abs/2017A

    Shimwell T. W., et al., 2017, @doi [ ] 10.1051/0004-6361/201629313 , http://adsabs.harvard.edu/abs/2017A

    2017 doi

  68. [76]

    W., et al., 2019, @doi [ ] 10.1051/0004-6361/201833559 , https://ui.adsabs.harvard.edu/abs/2019A&A...622A...1S 622, A1

    Shimwell T. W., et al., 2019, @doi [ ] 10.1051/0004-6361/201833559 , https://ui.adsabs.harvard.edu/abs/2019A&A...622A...1S 622, A1

    2019 doi

  69. [77]

    I., 1963, @doi [ ] 10.1038/199682a0 , http://adsabs.harvard.edu/abs/1963Natur.199..682S 199, 682

    Slish V. I., 1963, @doi [ ] 10.1038/199682a0 , http://adsabs.harvard.edu/abs/1963Natur.199..682S 199, 682

    1963 doi

  70. [78]

    V., Kovalev Y

    Sokolovsky K. V., Kovalev Y. Y., Pushkarev A. B., Mimica P., Perucho M., 2011, @doi [ ] 10.1051/0004-6361/201015772 , http://adsabs.harvard.edu/abs/2011A

    2011 doi

  71. [79]

    Spoelstra T. A. T., Patnaik A. R., Gopal-Krishna 1985, , http://adsabs.harvard.edu/abs/1985A

    1985

  72. [80]

    P., Baum S

    Stanghellini C., Dallacasa D., O'Dea C. P., Baum S. A., Fanti R., Fanti C., 2001, @doi [ ] 10.1051/0004-6361:20011101 , http://adsabs.harvard.edu/abs/2001A

    2001 doi

  73. [81]

    C., Moderski R., Kataoka J., Wagner S., 2008, @doi [ ] 10.1086/587781 , http://adsabs.harvard.edu/abs/2008ApJ...680..911S 680, 911

    Stawarz ., Ostorero L., Begelman M. C., Moderski R., Kataoka J., Wagner S., 2008, @doi [ ] 10.1086/587781 , http://adsabs.harvard.edu/abs/2008ApJ...680..911S 680, 911

    2008 doi

  74. [82]

    K., Rao A

    Swarup G., Ananthakrishnan S., Kapahi V. K., Rao A. P., Subrahmanya C. R., Kulkarni V. K., 1991, Current Science, Vol. 60, NO.2/JAN25, P. 95, 1991, http://adsabs.harvard.edu/abs/1991CuSc...60...95S 60, 95

    1991

  75. [83]

    B., et al., 2005, @doi [ ] 10.1086/430255 , http://adsabs.harvard.edu/abs/2005ApJS..159...27T 159, 27

    Taylor G. B., et al., 2005, @doi [ ] 10.1086/430255 , http://adsabs.harvard.edu/abs/2005ApJS..159...27T 159, 27

    2005 doi

  76. [84]

    J., Murphy D

    Tingay S. J., Murphy D. W., 2001, @doi [ ] 10.1086/318247 , http://adsabs.harvard.edu/abs/2001ApJ...546..210T 546, 210

    2001 doi

  77. [85]

    J., de Kool M., 2003, @doi [ ] 10.1086/376600 , http://adsabs.harvard.edu/abs/2003AJ....126..723T 126, 723

    Tingay S. J., de Kool M., 2003, @doi [ ] 10.1086/376600 , http://adsabs.harvard.edu/abs/2003AJ....126..723T 126, 723

    2003 doi

  78. [86]

    C., Ros E., Kellermann K

    Vermeulen R. C., Ros E., Kellermann K. I., Cohen M. H., Zensus J. A., van Langevelde H. J., 2003, @doi [ ] 10.1051/0004-6361:20021752 , http://adsabs.harvard.edu/abs/2003A

    2003 doi

  79. [87]

    V \'e ron-Cetty M.-P., V \'e ron P., 2010, @doi [ ] 10.1051/0004-6361/201014188 , http://adsabs.harvard.edu/abs/2010A

    2010 doi

  80. [88]

    C., Romney J

    Walker R. C., Romney J. D., Benson J. M., 1994, in Zensus J. A., Kellermann K. I., eds, Compact Extragalactic Radio Sources. p. 121

    1994

  81. [89]

    B., et al., 2015, @doi [ ] 10.1017/pasa.2015.26 , http://adsabs.harvard.edu/abs/2015PASA...32...25W 32, e025

    Wayth R. B., et al., 2015, @doi [ ] 10.1017/pasa.2015.26 , http://adsabs.harvard.edu/abs/2015PASA...32...25W 32, e025

    2015 doi

  82. [90]

    N., Polatidis A

    Wilkinson P. N., Polatidis A. G., Readhead A. C. S., Xu W., Pearson T. J., 1994, @doi [ ] 10.1086/187518 , http://adsabs.harvard.edu/abs/1994ApJ...432L..87W 432, L87

    1994 doi

  83. [91]

    Xu W., Readhead A. C. S., Pearson T. J., Polatidis A. G., Wilkinson P. N., 1995, @doi [ ] 10.1086/192189 , http://adsabs.harvard.edu/abs/1995ApJS...99..297X 99, 297

    1995 doi

  84. [92]

    Zovaro H. R. M., Sharp R., Nesvadba N. P. H., Bicknell G. V., Mukherjee D., Wagner A. e. Y., Groves B., Krishna S., 2019, @doi [ ] 10.1093/mnras/stz233 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.3393Z 484, 3393

    2019 doi

  85. [93]

    de Bruyn G., et al., 2000, VizieR Online Data Catalog, http://adsabs.harvard.edu/abs/2000yCat.8062....0D 8062

    2000

  86. [94]

    C., 1989, @doi [ ] 10.1038/338484a0 , http://adsabs.harvard.edu/abs/1989Natur.338..484D 338, 484

    de Kool M., Begelman M. C., 1989, @doi [ ] 10.1038/338484a0 , http://adsabs.harvard.edu/abs/1989Natur.338..484D 338, 484

    1989 doi

  87. [95]

    H., Barthel P

    de Vries W. H., Barthel P. D., O'Dea C. P., 1997, , http://adsabs.harvard.edu/abs/1997A

    1997

  88. [96]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.