The GRB fundamental plane and the GRB-SNe connection� Dr. Maria Giovanna Dainotti

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24-10-2023, Palermo, Italy, Anisotropies in Core Collapsar SNe

NAOJ, DIVISION OF SCIENCE

Outline of the talk

1. Introduction on Gamma Ray Bursts.
2. GRB correlations involving the plateau emission.
3. GRB-SNe connection.
4. Theoretical interpretation of GRB correlations.
5. Conclusions.

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GRB phenomenology

• Flashes of high energy photons in the sky (typical duration is few seconds).
• Isotropic distribution in the sky.
• Cosmological origin accepted (furthest GRBs observed z ~ 9.4 – 13.14 billions of light-years).
• Extremely energetic: the greatest amount of energy released in a short time (not considering the Big Bang).
• X-rays and optical and radio radiation observed after days/months (afterglows), distinct from the main γ-ray events (the prompt emission).

Afterglow

A well-sampled GRB light curve observed by Swift BAT+ XRT.

The blue line is the

phenomenological Willingale et al. (2007) model.

The gold sample

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Because They…

• Can be probes of the early evolution of the Universe.
• Are observed beyond the epoch of reionization.
• Allow us to investigate Pop III stars.
• Allow us to track the star formation.
• Are much more distant than SN Ia (z=2.26) and quasars (z=7).

But They…

• Don’t seem to be standard candles with their isotropic prompt luminosities spanning over 8 order of magnitudes.

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Why are GRBs potential cosmological tools?�

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Swift lightcurves taken from the Swift repository

For 20 years, we’ve been struggling: how to use GRBs as standard candles?

Challenge: Light curves vary widely - “if you've seen one GRB, you've seen one GRB” --

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Which GRB class works best as a standard candle?

GRB zoo

Alone, none of these classes are standard candles (but I have good news for you later).

Now the drive is to standardize them.

compact object mergers (NS-NS, NS-BH)

core collapse of massive stars

(M > 30 M_sun)

La-Ta correlation first discovered by Dainotti, et al. (2008), MNRAS, 391, L 79D, later updated by Dainotti et al. (2010), ApJL, 722, L 215; Dainotti et al. (2011a), ApJ, 730, 135; Dainotti et al. (2015a), ApJ, 800, 1, 31. The La-Lpeak first discovered by Dainotti et al., MNRAS, 2011b, 418, 2202.

Possible reliable candidates are the and Lpeak-La correlations

Black -> z < 0.89

Magenta -> 0.89 ≤ z ≤ 1.68 Blue -> 1.68 < z ≤ 2.45 Green -> 2.45 < z ≤ 3.45

Red -> z ≥ 3.45.

To account for selection biases Dainotti et al. 2013, ApJ, 774, 157 and Dainotti et al. 2015b, MNRAS, 451, 4 showed that both these correlations are intrinsic to GRB physics and not to selection biases.

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b=-1.0 -> Energy reservoir of the plateau is constant

Log Lx(Ta)= log A +B log Lpeak

Blue -> z ≤ 0.84

Magenta -> 0.84 ≤ z ≤ 1.8 Green -> 1.8 < z ≤ 2.9

Red -> z ≥ 2.9.

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Long GRBs - blue points- for which the SNe has not been seen�GRB-SNe associated - red triangles�Long-GRB-NO-SNe at low z - black filled triangle

Hunting a more homogeneous sample

for a “standard GRB set for cosmology”

• The difference between the 2 slopes

GRB-SNe and GRB-LONG-NO-SNe is 2.8 sigma with P=0.045

• b=-1.9 slope of GRB-SNe -> the plateau energy reservoir is not constant
• SNe-GRBs sample is also taken by Cano et al. 2014, A&A, 568,19.
• The GRB-SNe Ib/c connection is important for ongoing and future projects.

Dainotti, Nagataki, Maeda, Postnikov & Pian, 2017 A&A, 600, id. A98, 11

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• the 3D Lpeak-Lx-Ta correlation is intrinsic and it has a reduced scatter, σint of 24 %.

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AN EXTENSION OF THE LX-TA AND LX-LPEAK CORRELATIONS GIVEN THEIR INTRINSIC NATURE

X-ray Flashes

GRB-SNe

Short

Long

Dainotti, Postnikov, Hernandez, Ostrowski 2016, ApJL, 825L, 20

Press release by NASA:

https://swift.gsfc.nasa.gov/news/2016/grbs_std_candles.html

Mention in Scientific American, Stanford highlight of 2016, INAF Blogs, UNAM gaceta, and many online newspapers took the news.

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The gold sample (40 GRBs) :

Flat plateau (< 41°)

At least 5 points at the plateaus’ beginning

The gold sample reduces σint of 54% compared

to the 2D correlation for 122 long GRBs

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Distance from the planes

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�D Dainotti, Hernandez, Postnikov, Nagataki, Obrien, Willingale, Striegel, 2017, ApJ, 848, 88 848,88

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• Press releases by INAF, Nature-Index, a research highlight at Stanford, and Le Scienze (Scientific American in italian):� http://www.inaf.it/en/inaf-news/gold-grb#null�

https://www.facebook.com/Marie.Curie.Actions/photos/a.443662259040646/2766583496748499/?type=3&theater

Interviewed by the Italian National daily news on Women day

Marie Curie Fellow of the week

5-12 May 2018

Total sample of 184 GRBs

the gold sample fundamental plane is a reference (placed in 0). The gold sample has the smallest scatter.

Black=Long GRBs

Red=Short GRBs

Blue=XRFs

Orange=GRB-SNe

Purple=gold sample

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Fallback accretion onto a black hole

Spinning down of a magnetar

The GRB plateau emission can be described through two models:

A. Rowlinson, et al., 2014, MNRAS, 443, 2, 1779-1787

P. Kumar, et al., 2008, MNRAS, 388, 4, 1729-1742

The physical interpretation of the plateau

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Two different classes within the magnetar scenario

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• The spin-down luminosity of the magnetar is entirely beamed within Ɵjet.

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• The long GRB 070208 (circle) and the peculiar GRB 060614A (square).

• Previous literature: Dall’Osso et al. 2011, Bernardini et al. 2012, 2013, 2015, Rowlinson et al. 2014 including Dainotti, Rea et al. 2015 (ncluding Dainotti), Beniamini et al. 2017, Beniamini & Mochkovitch 2017.

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• Within the external shock model (Srinivasagaravan, Dainotti et al. 2020, Warren et al. 2017).

Stratta, Dainotti, Dall’Osso, Hernandez, de Cesare 2018, ApJ, 869, 155

Why a beamed jet is preferred to isotropic emission

• This is also supported by detailed numerical simulations of proto-magnetar (PM) formation (Obergaulinger & Aloy 2017).
• Obergaulinger & Aloy 2017 strongly suggests that
• (1) the formation of a PM is preceded by the ejection of a highly collimated outflow,
• (2) the environment surrounding the PM is highly anisotropic, with a large variation in properties from the direction of the rotational axis to the equatorial region, and
• (3) the maximum rotational energy that may be stored (and hence constitutes the energy reservoir for the magnetar spin-down) can be significantly larger than previously suggested limits and consistent with the values here.
• Both the collimated ejecta and the anisotropy of the medium surrounding the PM may certainly have an impact on the observed distribution of the spin-down energy. This provides a possible interpretation as to why our fits suggest a preference for a collimated spin-down.

Conclusions I: towards standard candles

• The 3D correlation for the gold sample has a σint 54% smaller than the long GRBs for the Lx-Ta correlation.

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It is the tightest three parameter correlation including the plateau phase.

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• The statistical difference of the planes of short and long GRBs

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a difference in the B, P diagram of the magnetars.

• It also holds for Fermi-GBM bursts.

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For a more a complete review see

Dainotti & Amati,

“Gamma Ray Burst selection effects in prompt correlations: an overview”,

PASP, 30, 987, 051001 (2018b).

A series of review papers:

Dainotti, M.G., del Vecchio, R. & Tarnopolski, M.,

“Gamma Ray Burst Prompt correlations” Advances in Astronomy, vol. 2018, id. 4969503.

Dainotti, M.G., & del Vecchio, R.,

“Gamma Ray Burst afterglow and prompt-afterglow relations: An overview”,

NAREV, 77, 23 (2017).

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The fundamental plane relation for new classes: Ambushing the standard candle in its own nest

• The platinum sample: a subset of the gold sample obtained after removing gold GRBs with at least one of the following features:
• Tx is inside a large gap of the data, and thus has a large uncertainty.
• A small plateau duration <500 s with gaps after it. This could mean that the plateau phase is longer than the one observed.
• Flares and bumps at the start and during the plateau phase.
• It reduces the scatter of 31%.

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Dainotti, Lenart, Sarracino, Nagataki, Capozziello & Fraija 2020, ApJ, 904, issue 2, 97, 13

Press release distributed by the AAS, issued by Jagiellonian, Space Science Institute, and by INAF

(Italian National Astrophysics Institute) and interview by INAF.

The fundamental plane relation for new classes

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• KNe are transient objects which are derived by the mergers of two neutron stars.
• Several KN have been associated with short GRBs.
• All cases are presented in Rossi et al. 2020.
• The total sample is composed of 222 GRBs

Dainotti et al. 2020, ApJ, 904, issue 2, 97, 13

3D fundamental plane relations for different samples: �the whole, GRBs associated with KNe and SGRB and KNe.

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Dainotti et al. 2020, ApJ, 904, issue 2, 97, 13

All 222 GRBs with plateaus

GRBs associated with KNe

SGRBs and SGRBs-KNe

The distances from the Gold fundamental plane

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A Z-score is measured in terms of standard deviations from the mean.

If Z=0, the score is identical to the mean score.

Dainotti et al. 2020, ApJ, 904, issue 2, 97, 13.

What happens to the GRB-SNe connection with the fundamental plane in optical?

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The 3D correlation in optical exists for 58 GRBs !!!� M. G. Dainotti, et al., 2022c, ApJS, 261, 2, 25. Press release from NAOJ

• Long=31
• Gold🡪 6
• XRF=4
• XRR=19
• GRB-SNe Ib/c-> 9
• SNe Ib/c (ABC)->7

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The difference and similarities in the parameters

How can we investigate further and more generally the GRB-SNe connection?

GRB and SNe correlations

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The search of intrinsic correlations between the parameters of GRBs and SNe.

GRB-GRB parameters correlations

- Amati et al. 2002 (Ep-Eiso)

- Yonetoku et al. 2004 (Ep-Lpeak)

- Ghirlanda et al. 2004 (Ep-Egamma)

- Oates et al. 2012 (brightness-decay rate for UVOT GRBs)

- Tsutsui & Shigeyama 2013 (scaling law)

- Dainotti et al. 2008, 2020b (time and luminosity of plateau-end in X-rays and optical)

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Amati, Ghirlanda, Tsutsui, and Dainotti relations work also for GRB-SNe

GRB(prompt)-SN parameters correlations

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- Li et al. 2006a (Ep-bolometric magnitude)�- Lü et al. 2018 (Ep-nickel mass)

SN-SN parameters

correlations(*)

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- Cano 2014 (s-k)

GRB(afterglow)-SN parameters correlations(?)

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Missing in the previous literature

(*) in the case of SNe associated with GRBs

Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

Our contribution

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In our quest for GRB-SN parameter correlations, we leveraged the following:

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• The collection of the most complete catalogue of GRB-SNe events so far observed (from 1991 to February 2021)

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• The presence of the afterglow properties (the X-rays and optical plateau phases for 15 and 20 GRBs, respectively)

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• A reliable statistical method for the correction of selection biases that may affect the GRB and SN parameters: the Efron and Petrosian method (EP method, Efron & Petrosian 1992)

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We performed a systematic research for correlations among all the known parameters of GRB-SNe with restrictive metrics.

Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

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Dainotti et al. 2022e

Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

The catalogue

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Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

The parameters

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Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

The Efron and Petrosian method

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Dainotti et al. 2022e

Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

The metrics and the fitting

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Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

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Dainotti et al. 2022e

Red=AB

Green=E

Red=AB

Green=E

Before EP correction

After EP correction

Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

Discussion and conclusion

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• We cross-related all the GRB and SN parameters for a sample of 69 GRB-SNe associations, thus testing 91 bidimensional correlations

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• The parameters in our total sample were corrected for selection biases and redshift evolution through the EP method

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• The hint of the correlation that we found between the optical plateau-end luminosity for the GRBs and the rest-frame peak time shows how the brightest GRB plateaus are accompanied by the most delayed SNe. Furthermore, the peak time of a SN is linked to the diffusion time (Khatami & Kasen 2019) which, in turn, is related to the width of the LC.

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• The future observations of GRB-SNe events with satellites and ground telescopes (such as KISO and Subaru) are expected to provide more evidence and their data are waited to check if the probable correlation can be confirmed

Maria Giovanna Dainotti, National Astronomical Observatory of Japan & SOKENDAI, maria.dainotti@nao.ac.jp

What else do we need for GRB-SNe connection?

New or tighter Reliable correlations

How?

Increase the sample size

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Physical interpretation, connection with theory

In the quest for the standard set�

With machine learning

For redshift inference, regression:

1) Dainotti, Narendra, Pollo et al. 2021, ApJ,920, 2, 118.

2) Narendra, Gibson, Dainotti, Pollo et al. 2022, ApJS, 259, 2, 55.

3) Gibson, Narendra, Dainotti, Pollo et al. 2022, Frontiers in Astronomy and Space Science, 9, 836215

4) Lightcurve Reconstruction, Dainotti, including Narendra, Pollo et al. 2023, ApJS�2023arXiv230512126D

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